This document summarizes research on reconstructing past atmospheric oxygen (O2) levels over the past 800,000 years using O2/N2 ratios measured from ancient air bubbles trapped in ice cores from Greenland and Antarctica. The main findings are:
1) O2/N2 ratios from multiple ice cores show a consistent decline of 8.4‰ per million years over the past 800,000 years, equivalent to a 0.7% decline in atmospheric O2 levels.
2) This decline is unlikely to be explained by changes in air bubble formation processes or other non-atmospheric factors, as argon/nitrogen ratios from the same ice cores show an inconsistent increasing trend over the same
Observed glacier and volatile distribution on Pluto from atmosphere–topograph...Sérgio Sacani
Pluto has a variety of surface frosts and landforms as well as a
complex atmosphere1. There is ongoing geological activity related
to the massive Sputnik Planum glacier, mostly made of nitrogen (N2)
ice mixed with solid carbon monoxide and methane2, covering the
4-kilometre-deep, 1,000-kilometre-wide basin of Sputnik Planum1,3
near the anti-Charon point. The glacier has been suggested to arise
from a source region connected to the deep interior, or from a sink
collecting the volatiles released planetwide1. Thin deposits of N2
frost, however, were also detected at mid-northern latitudes and
methane ice was observed to cover most of Pluto except for the
darker, frost-free equatorial regions2. Here we report numerical
simulations of the evolution of N2, methane and carbon monoxide
on Pluto over thousands of years. The model predicts N2 ice
accumulation in the deepest low-latitude basin and the threefold
increase in atmospheric pressure that has been observed to occur
since 19884–6. This points to atmospheric–topographic processes as
the origin of Sputnik Planum’s N2 glacier. The same simulations also
reproduce the observed quantities of volatiles in the atmosphere and
show frosts of methane, and sometimes N2, that seasonally cover the
mid- and high latitudes, explaining the bright northern polar cap
reported in the 1990s7,8 and the observed ice distribution in 20152.
The model also predicts that most of these seasonal frosts should
disappear in the next decade.
T he effect_of_orbital_configuration)_on_the_possible_climates_and_habitabili...Sérgio Sacani
As lower-mass stars often host multiple rocky planets, gravitational interactions among planets can have significant
effects on climate and habitability over long timescales. Here we explore a specific case, Kepler-62f (Borucki et al.,
2013), a potentially habitable planet in a five-planet system with a K2V host star. N-body integrations reveal the
stable range of initial eccentricities for Kepler-62f is 0.00 £ e £ 0.32, absent the effect of additional, undetected
planets. We simulate the tidal evolution of Kepler-62f in this range and find that, for certain assumptions, the planet
can be locked in a synchronous rotation state. Simulations using the 3-D Laboratoire de Me´te´orologie Dynamique
(LMD) Generic global climate model (GCM) indicate that the surface habitability of this planet is sensitive to
orbital configuration.With 3 bar of CO2 in its atmosphere, we find that Kepler-62f would only be warm enough for
surface liquid water at the upper limit of this eccentricity range, providing it has a high planetary obliquity
(between 60 and 90). A climate similar to that of modern-day Earth is possible for the entire range of stable
eccentricities if atmospheric CO2 is increased to 5 bar levels. In a low-CO2 case (Earth-like levels), simulations
with version 4 of the Community Climate System Model (CCSM4) GCM and LMD Generic GCM indicate that
increases in planetary obliquity and orbital eccentricity coupled with an orbital configuration that places the
summer solstice at or near pericenter permit regions of the planet with above-freezing surface temperatures. This
may melt ice sheets formed during colder seasons. If Kepler-62f is synchronously rotating and has an ocean, CO2
levels above 3 bar would be required to distribute enough heat to the nightside of the planet to avoid atmospheric
freeze-out and permit a large enough region of open water at the planet’s substellar point to remain stable. Overall,
we find multiple plausible combinations of orbital and atmospheric properties that permit surface liquid water on
Kepler-62f. Key Words: Extrasolar planets—Habitability—Planetary environments. Astrobiology 16, xxx–xxx.
Evidence for plumes of water on Europa has previously been found using the Hubble Space Telescope using two
different observing techniques. Roth et al. found line emission from the dissociation products of water. Sparks et al.
found evidence for off-limb continuum absorption as Europa transited Jupiter. Here, we present a new transit
observation of Europa that shows a second event at the same location as a previous plume candidate from Sparks
et al., raising the possibility of a consistently active source of erupting material on Europa. This conclusion is
bolstered by comparison with a nighttime thermal image from the Galileo Photopolarimeter-Radiometer that shows
a thermal anomaly at the same location, within the uncertainties. The anomaly has the highest observed brightness
temperature on the Europa nightside. If heat flow from a subsurface liquid water reservoir causes the thermal
anomaly, its depth is ≈1.8–2 km, under simple modeling assumptions, consistent with scenarios in which a liquid
water reservoir has formed within a thick ice shell. Models that favor thin regions within the ice shell that connect
directly to the ocean, however, cannot be excluded, nor modifications to surface thermal inertia by subsurface
activity. Alternatively, vapor deposition surrounding an active vent could increase the thermal inertia of the surface
and cause the thermal anomaly. This candidate plume region may offer a promising location for an initial
characterization of Europa’s internal water and ice and for seeking evidence of Europa’s habitability.
Cassini finds molecular hydrogen in the Enceladus plume: Evidence for hydroth...Sérgio Sacani
Saturn’s moon Enceladus has an ice-covered ocean; a plume of material erupts from
cracks in the ice. The plume contains chemical signatures of water-rock interaction
between the ocean and a rocky core.We used the Ion Neutral Mass Spectrometer onboard
the Cassini spacecraft to detect molecular hydrogen in the plume. By using the instrument’s
open-source mode, background processes of hydrogen production in the instrument were
minimized and quantified, enabling the identification of a statistically significant signal of
hydrogen native to Enceladus.We find that the most plausible source of this hydrogen is
ongoing hydrothermal reactions of rock containing reduced minerals and organic materials.
The relatively high hydrogen abundance in the plume signals thermodynamic disequilibrium
that favors the formation of methane from CO2 in Enceladus’ ocean.
PROBING FOR EVIDENCE OF PLUMES ON EUROPA WITH HST/STISSérgio Sacani
Roth et al. (2014a) reported evidence for plumes of water venting from a southern high latitude
region on Europa – spectroscopic detection of off-limb line emission from the dissociation
products of water. Here, we present Hubble Space Telescope (HST) direct images of Europa in
the far ultraviolet (FUV) as it transited the smooth face of Jupiter, in order to measure absorption
from gas or aerosols beyond the Europa limb. Out of ten observations we found three in which
plume activity could be implicated. Two show statistically significant features at latitudes similar
to Roth et al., and the third, at a more equatorial location. We consider potential systematic
effects that might influence the statistical analysis and create artifacts, and are unable to find any
that can definitively explain the features, although there are reasons to be cautious. If the
apparent absorption features are real, the magnitude of implied outgassing is similar to that of the
Roth et al. feature, however the apparent activity appears more frequently in our data.
Meridional brightness temperatures were measured on the surface of Titan during the 2004–2014 portion of the
Cassini mission by the Composite Infrared Spectrometer. Temperatures mapped from pole to pole during five twoyear
periods show a marked seasonal dependence. The surface temperature near the south pole over this time
decreased by 2 K from 91.7±0.3 to 89.7±0.5 K while at the north pole the temperature increased by 1 K from
90.7±0.5 to 91.5±0.2 K. The latitude of maximum temperature moved from 19 S to 16 N, tracking the subsolar
latitude. As the latitude changed, the maximum temperature remained constant at 93.65±0.15 K. In 2010
our temperatures repeated the north–south symmetry seen by Voyager one Titan year earlier in 1980. Early in the
mission, temperatures at all latitudes had agreed with GCM predictions, but by 2014 temperatures in the north were
lower than modeled by 1 K. The temperature rise in the north may be delayed by cooling of sea surfaces and moist
ground brought on by seasonal methane precipitation and evaporation.
Observed glacier and volatile distribution on Pluto from atmosphere–topograph...Sérgio Sacani
Pluto has a variety of surface frosts and landforms as well as a
complex atmosphere1. There is ongoing geological activity related
to the massive Sputnik Planum glacier, mostly made of nitrogen (N2)
ice mixed with solid carbon monoxide and methane2, covering the
4-kilometre-deep, 1,000-kilometre-wide basin of Sputnik Planum1,3
near the anti-Charon point. The glacier has been suggested to arise
from a source region connected to the deep interior, or from a sink
collecting the volatiles released planetwide1. Thin deposits of N2
frost, however, were also detected at mid-northern latitudes and
methane ice was observed to cover most of Pluto except for the
darker, frost-free equatorial regions2. Here we report numerical
simulations of the evolution of N2, methane and carbon monoxide
on Pluto over thousands of years. The model predicts N2 ice
accumulation in the deepest low-latitude basin and the threefold
increase in atmospheric pressure that has been observed to occur
since 19884–6. This points to atmospheric–topographic processes as
the origin of Sputnik Planum’s N2 glacier. The same simulations also
reproduce the observed quantities of volatiles in the atmosphere and
show frosts of methane, and sometimes N2, that seasonally cover the
mid- and high latitudes, explaining the bright northern polar cap
reported in the 1990s7,8 and the observed ice distribution in 20152.
The model also predicts that most of these seasonal frosts should
disappear in the next decade.
T he effect_of_orbital_configuration)_on_the_possible_climates_and_habitabili...Sérgio Sacani
As lower-mass stars often host multiple rocky planets, gravitational interactions among planets can have significant
effects on climate and habitability over long timescales. Here we explore a specific case, Kepler-62f (Borucki et al.,
2013), a potentially habitable planet in a five-planet system with a K2V host star. N-body integrations reveal the
stable range of initial eccentricities for Kepler-62f is 0.00 £ e £ 0.32, absent the effect of additional, undetected
planets. We simulate the tidal evolution of Kepler-62f in this range and find that, for certain assumptions, the planet
can be locked in a synchronous rotation state. Simulations using the 3-D Laboratoire de Me´te´orologie Dynamique
(LMD) Generic global climate model (GCM) indicate that the surface habitability of this planet is sensitive to
orbital configuration.With 3 bar of CO2 in its atmosphere, we find that Kepler-62f would only be warm enough for
surface liquid water at the upper limit of this eccentricity range, providing it has a high planetary obliquity
(between 60 and 90). A climate similar to that of modern-day Earth is possible for the entire range of stable
eccentricities if atmospheric CO2 is increased to 5 bar levels. In a low-CO2 case (Earth-like levels), simulations
with version 4 of the Community Climate System Model (CCSM4) GCM and LMD Generic GCM indicate that
increases in planetary obliquity and orbital eccentricity coupled with an orbital configuration that places the
summer solstice at or near pericenter permit regions of the planet with above-freezing surface temperatures. This
may melt ice sheets formed during colder seasons. If Kepler-62f is synchronously rotating and has an ocean, CO2
levels above 3 bar would be required to distribute enough heat to the nightside of the planet to avoid atmospheric
freeze-out and permit a large enough region of open water at the planet’s substellar point to remain stable. Overall,
we find multiple plausible combinations of orbital and atmospheric properties that permit surface liquid water on
Kepler-62f. Key Words: Extrasolar planets—Habitability—Planetary environments. Astrobiology 16, xxx–xxx.
Evidence for plumes of water on Europa has previously been found using the Hubble Space Telescope using two
different observing techniques. Roth et al. found line emission from the dissociation products of water. Sparks et al.
found evidence for off-limb continuum absorption as Europa transited Jupiter. Here, we present a new transit
observation of Europa that shows a second event at the same location as a previous plume candidate from Sparks
et al., raising the possibility of a consistently active source of erupting material on Europa. This conclusion is
bolstered by comparison with a nighttime thermal image from the Galileo Photopolarimeter-Radiometer that shows
a thermal anomaly at the same location, within the uncertainties. The anomaly has the highest observed brightness
temperature on the Europa nightside. If heat flow from a subsurface liquid water reservoir causes the thermal
anomaly, its depth is ≈1.8–2 km, under simple modeling assumptions, consistent with scenarios in which a liquid
water reservoir has formed within a thick ice shell. Models that favor thin regions within the ice shell that connect
directly to the ocean, however, cannot be excluded, nor modifications to surface thermal inertia by subsurface
activity. Alternatively, vapor deposition surrounding an active vent could increase the thermal inertia of the surface
and cause the thermal anomaly. This candidate plume region may offer a promising location for an initial
characterization of Europa’s internal water and ice and for seeking evidence of Europa’s habitability.
Cassini finds molecular hydrogen in the Enceladus plume: Evidence for hydroth...Sérgio Sacani
Saturn’s moon Enceladus has an ice-covered ocean; a plume of material erupts from
cracks in the ice. The plume contains chemical signatures of water-rock interaction
between the ocean and a rocky core.We used the Ion Neutral Mass Spectrometer onboard
the Cassini spacecraft to detect molecular hydrogen in the plume. By using the instrument’s
open-source mode, background processes of hydrogen production in the instrument were
minimized and quantified, enabling the identification of a statistically significant signal of
hydrogen native to Enceladus.We find that the most plausible source of this hydrogen is
ongoing hydrothermal reactions of rock containing reduced minerals and organic materials.
The relatively high hydrogen abundance in the plume signals thermodynamic disequilibrium
that favors the formation of methane from CO2 in Enceladus’ ocean.
PROBING FOR EVIDENCE OF PLUMES ON EUROPA WITH HST/STISSérgio Sacani
Roth et al. (2014a) reported evidence for plumes of water venting from a southern high latitude
region on Europa – spectroscopic detection of off-limb line emission from the dissociation
products of water. Here, we present Hubble Space Telescope (HST) direct images of Europa in
the far ultraviolet (FUV) as it transited the smooth face of Jupiter, in order to measure absorption
from gas or aerosols beyond the Europa limb. Out of ten observations we found three in which
plume activity could be implicated. Two show statistically significant features at latitudes similar
to Roth et al., and the third, at a more equatorial location. We consider potential systematic
effects that might influence the statistical analysis and create artifacts, and are unable to find any
that can definitively explain the features, although there are reasons to be cautious. If the
apparent absorption features are real, the magnitude of implied outgassing is similar to that of the
Roth et al. feature, however the apparent activity appears more frequently in our data.
Meridional brightness temperatures were measured on the surface of Titan during the 2004–2014 portion of the
Cassini mission by the Composite Infrared Spectrometer. Temperatures mapped from pole to pole during five twoyear
periods show a marked seasonal dependence. The surface temperature near the south pole over this time
decreased by 2 K from 91.7±0.3 to 89.7±0.5 K while at the north pole the temperature increased by 1 K from
90.7±0.5 to 91.5±0.2 K. The latitude of maximum temperature moved from 19 S to 16 N, tracking the subsolar
latitude. As the latitude changed, the maximum temperature remained constant at 93.65±0.15 K. In 2010
our temperatures repeated the north–south symmetry seen by Voyager one Titan year earlier in 1980. Early in the
mission, temperatures at all latitudes had agreed with GCM predictions, but by 2014 temperatures in the north were
lower than modeled by 1 K. The temperature rise in the north may be delayed by cooling of sea surfaces and moist
ground brought on by seasonal methane precipitation and evaporation.
On the possibility of through passage of asteroid bodies across the Earth’s a...Sérgio Sacani
We have studied the conditions of through passage of asteroids with diameters 200, 100, and
50 m, consisting of three types of materials – iron, stone, and water ice, across the Earth’s
atmosphere with a minimum trajectory altitude in the range 10–15 km. The conditions of this
passage with a subsequent exit into outer space with the preservation of a substantial fraction
of the initial mass have been found. The results obtained support our idea explaining one of the
long-standing problems of astronomy – the Tunguska phenomenon, which has not received
reasonable and comprehensive interpretations to date. We argue that the Tunguska event was
caused by an iron asteroid body, which passed through the Earth’s atmosphere and continued
to the near-solar orbit.
High-resolution UV/Optical/IR Imaging of Jupiter in 2016–2019Sérgio Sacani
Imaging observations of Jupiter with high spatial resolution were acquired beginning in 2016, with a cadence of 53
days to coincide with atmospheric observations of the Juno spacecraft during each perijove pass. The Wide Field
Camera 3 (WFC3) aboard the Hubble Space Telescope (HST) collected Jupiter images from 236 to 925 nm in 14
filters. The Near-Infrared Imager (NIRI) at Gemini North imaged Jovian thermal emission using a lucky-imaging
approach (co-adding the sharpest frames taken from a sequence of short exposures), using the M′ filter at 4.7 μm.
We discuss the data acquisition and processing and an archive collection that contains the processed WFC3 and
NIRI data (doi:10.17909/T94T1H). Zonal winds remain steady over time at most latitudes, but significant
evolution of the wind profile near 24°N in 2016 and near 15°S in 2017 was linked with convective superstorm
eruptions. Persistent mesoscale waves were seen throughout the 2016–2019 period. We link groups of lightning
flashes observed by the Juno team with water clouds in a large convective plume near 15°S and in cyclones near
35°N–55°N. Thermal infrared maps at the 10.8 micron wavelength obtained at the Very Large Telescope show
consistent high brightness temperature anomalies, despite a diversity of aerosol properties seen in the HST data.
Both WFC3 and NIRI imaging reveal depleted aerosols consistent with downwelling around the periphery of the
15°S storm, which was also observed by the Atacama Large Millimeter/submillimeter Array. NIRI imaging of
the Great Red Spot shows that locally reduced cloud opacity is responsible for dark features within the vortex. The
HST data maps multiple concentric polar hoods of high-latitude hazes.
Artigo descreve como os cientistas utilizaram o Telescópio Espacial Hubble para descobrir a estratosfera num exoplaneta classificado como um Júpiter quente. Descoberta essa que pode ajudar a descobrir como os exoplanetas se formam e qual a composição de suas atmosferas.
SPECTROSCOPIC CONFIRMATION OF THE EXISTENCE OF LARGE, DIFFUSE GALAXIES IN THE...Sérgio Sacani
We recently identified a population of low surface brightness objects in the field of the z = 0.023 Coma cluster,
using the Dragonfly Telephoto Array. Here we present Keck spectroscopy of one of the largest of these “ultradiffuse
galaxies” (UDGs), confirming that it is a member of the cluster. The galaxy has prominent absorption
features, including the Ca II H+K lines and the G-band, and no detected emission lines. Its radial velocity of
cz=6280±120 km s−1 is within the 1σ velocity dispersion of the Coma cluster. The galaxy has an effective
radius of 4.3 ± 0.3 kpc and a Sérsic index of 0.89 ± 0.06, as measured from Keck imaging. We find no indications
of tidal tails or other distortions, at least out to a radius of ∼2re. We show that UDGs are located in a previously
sparsely populated region of the size—magnitude plane of quiescent stellar systems, as they are ∼6 mag fainter
than normal early-type galaxies of the same size. It appears that the luminosity distribution of large quiescent
galaxies is not continuous, although this could largely be due to selection effects. Dynamical measurements are
needed to determine whether the dark matter halos of UDGs are similar to those of galaxies with the same
luminosity or to those of galaxies with the same size.
The importance of comets for the origin of life on Earth has been advocated for many decades. Amino acids are
key ingredients in chemistry, leading to life as we know it. Many primitive meteorites contain amino acids, and it
is generally believed that these are formed by aqueous alterations. In the collector aerogel and foil samples of the
Stardust mission after the flyby at comet Wild 2, the simplest form of amino acids, glycine, has been found
together with precursor molecules methylamine and ethylamine. Because of contamination issues of the samples,
a cometary origin was deduced from the 13C isotopic signature. We report the presence of volatile glycine
accompanied by methylamine and ethylamine in the coma of 67P/Churyumov-Gerasimenko measured by
the ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) mass spectrometer, confirming the
Stardust results. Together with the detection of phosphorus and a multitude of organic molecules, this result
demonstrates that comets could have played a crucial role in the emergence of life on Earth.
Evidence for the_thermal_sunyaev-zeldovich_effect_associated_with_quasar_feed...Sérgio Sacani
Using a radio-quiet subsample of the Sloan Digital Sky Survey spectroscopic quasar
catalogue, spanning redshifts 0.5–3.5, we derive the mean millimetre and far-infrared
quasar spectral energy distributions (SEDs) via a stacking analysis of Atacama Cosmology
Telescope and Herschel-Spectral and Photometric Imaging REceiver data. We
constrain the form of the far-infrared emission and find 3σ–4σ evidence for the thermal
Sunyaev-Zel’dovich (SZ) effect, characteristic of a hot ionized gas component with
thermal energy (6.2 ± 1.7) × 1060 erg. This amount of thermal energy is greater than
expected assuming only hot gas in virial equilibrium with the dark matter haloes of
(1 − 5) × 1012h
−1M that these systems are expected to occupy, though the highest
quasar mass estimates found in the literature could explain a large fraction of this
energy. Our measurements are consistent with quasars depositing up to (14.5±3.3) τ
−1
8
per cent of their radiative energy into their circumgalactic environment if their typical
period of quasar activity is τ8 × 108 yr. For high quasar host masses, ∼ 1013h
−1M,
this percentage will be reduced. Furthermore, the uncertainty on this percentage is
only statistical and additional systematic uncertainties enter at the 40 per cent level.
The SEDs are dust dominated in all bands and we consider various models for dust
emission. While sufficiently complex dust models can obviate the SZ effect, the SZ
interpretation remains favoured at the 3σ–4σ level for most models.
WHERE IS THE FLUX GOING? THE LONG-TERM PHOTOMETRIC VARIABILITY OF BOYAJIAN’S ...Sérgio Sacani
We present ∼ 800 days of photometric monitoring of Boyajian’s Star (KIC 8462852) from the AllSky
Automated Survey for Supernovae (ASAS-SN) and ∼ 4000 days of monitoring from the All Sky
Automated Survey (ASAS). We show that from 2015 to the present the brightness of Boyajian’s Star
has steadily decreased at a rate of 6.3 ± 1.4 mmag yr−1
, such that the star is now 1.5% fainter than it
was in February 2015. Moreover, the longer time baseline afforded by ASAS suggests that Boyajian’s
Star has also undergone two brightening episodes in the past 11 years, rather than only exhibiting a
monotonic decline. We analyze a sample of ∼ 1000 comparison stars of similar brightness located in
the same ASAS-SN field and demonstrate that the recent fading is significant at & 99.4% confidence.
The 2015 − 2017 dimming rate is consistent with that measured with Kepler data for the time period
from 2009 to 2013. This long-term variability is difficult to explain with any of the physical models
for the star’s behavior proposed to date
A brief report on the interesting and exotic atmospheric phenomenon observed on extraterrestrial planets. this report is intended to go hand-in-hand with the presentation previous uploaded
TEMPORAL EVOLUTION OF THE HIGH-ENERGY IRRADIATION AND WATER CONTENT OF TRAPPI...Sérgio Sacani
The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting planets, some of which could
harbour liquid water on their surfaces. UV observations are essential to measure their high-energy
irradiation, and to search for photodissociated water escaping from their putative atmospheres. Our
new observations of TRAPPIST-1 Ly-α line during the transit of TRAPPIST-1c show an evolution of
the star emission over three months, preventing us from assessing the presence of an extended hydrogen
exosphere. Based on the current knowledge of the stellar irradiation, we investigated the likely history
of water loss in the system. Planets b to d might still be in a runaway phase, and planets within the
orbit of TRAPPIST-1g could have lost more than 20 Earth oceans after 8 Gyr of hydrodynamic escape.
However, TRAPPIST-1e to h might have lost less than 3 Earth oceans if hydrodynamic escape stopped
once they entered the habitable zone. We caution that these estimates remain limited by the large
uncertainty on the planet masses. They likely represent upper limits on the actual water loss because
our assumptions maximize the XUV-driven escape, while photodissociation in the upper atmospheres
should be the limiting process. Late-stage outgassing could also have contributed significant amounts
of water for the outer, more massive planets after they entered the habitable zone. While our results
suggest that the outer planets are the best candidates to search for water with the JWST, they also
highlight the need for theoretical studies and complementary observations in all wavelength domains
to determine the nature of the TRAPPIST-1 planets, and their potential habitability.
Keywords: planetary systems - Stars: individual: TRAPPIST-1
Very regular high-frequency pulsation modes in young intermediate-mass starsSérgio Sacani
Asteroseismology probes the internal structures of stars by using their natural
pulsation frequencies1. It relies on identifying sequences of pulsation modes that can
be compared with theoretical models, which has been done successfully for many
classes of pulsators, including low-mass solar-type stars2, red giants3, high-mass stars4
and white dwarfs5. However, a large group of pulsating stars of intermediate mass—the
so-called δ Scuti stars—have rich pulsation spectra for which systematic mode
identification has not hitherto been possible6,7. This arises because only a seemingly
random subset of possible modes are excited and because rapid rotation tends to
spoil regular patterns8–10. Here we report the detection of remarkably regular
sequences of high-frequency pulsation modes in 60 intermediate-mass
main-sequence stars, which enables definitive mode identification. The space
motions of some of these stars indicate that they are members of known associations
of young stars, as confirmed by modelling of their pulsation spectra.
EXTINCTION AND THE DIMMING OF KIC 8462852Sérgio Sacani
To test alternative hypotheses for the behavior of KIC 8462852, we obtained measurements of the star
over a wide wavelength range from the UV to the mid-infrared from October 2015 through December
2016, using Swift, Spitzer and at AstroLAB IRIS. The star faded in a manner similar to the longterm
fading seen in Kepler data about 1400 days previously. The dimming rate for the entire period
reported is 22.1 ± 9.7 milli-mag yr−1
in the Swift wavebands, with amounts of 21.0 ± 4.5 mmag in
the groundbased B measurements, 14.0 ± 4.5 mmag in V , and 13.0 ± 4.5 in R, and a rate of 5.0 ± 1.2
mmag yr−1 averaged over the two warm Spitzer bands. Although the dimming is small, it is seen at
& 3 σ by three different observatories operating from the UV to the IR. The presence of long-term
secular dimming means that previous SED models of the star based on photometric measurements
taken years apart may not be accurate. We find that stellar models with Tef f = 7000 - 7100 K and
AV ∼ 0.73 best fit the Swift data from UV to optical. These models also show no excess in the
near-simultaneous Spitzer photometry at 3.6 and 4.5 µm, although a longer wavelength excess from
a substantial debris disk is still possible (e.g., as around Fomalhaut). The wavelength dependence of
the fading favors a relatively neutral color (i.e., RV & 5, but not flat across all the bands) compared
with the extinction law for the general ISM (RV = 3.1), suggesting that the dimming arises from
circumstellar material
The future life span of Earth’s oxygenated atmosphereSérgio Sacani
Earth’s modern atmosphere is highly oxygenated and is a remotely detectable signal of
its surface biosphere. However, the lifespan of oxygen-based biosignatures in Earth’s
atmosphere remains uncertain, particularly for the distant future. Here we use a
combined biogeochemistry and climate model to examine the likely timescale of
oxygen-rich atmospheric conditions on Earth. Using a stochastic approach, we find that
the mean future lifespan of Earth’s atmosphere, with oxygen levels more than 1% of the
present atmospheric level, is 1.08 ± 0.14 billion years (1σ). The model projects that a
deoxygenation of the atmosphere, with atmospheric O2 dropping sharply to levels
reminiscent of the Archaean Earth, will most probably be triggered before the inception
of moist greenhouse conditions in Earth’s climate system and before the extensive loss
of surface water from the atmosphere. We find that future deoxygenation is an
inevitable consequence of increasing solar fluxes, whereas its precise timing is
modulated by the exchange flux of reducing power between the mantle and the ocean–
atmosphere–crust system. Our results suggest that the planetary carbonate–silicate cycle
will tend to lead to terminally CO2-limited biospheres and rapid atmospheric
deoxygenation, emphasizing the need for robust atmospheric biosignatures applicable
to weakly oxygenated and anoxic exoplanet atmospheres and highlighting the potential
importance of atmospheric organic haze during the terminal stages of planetary
habitability.
From our climate panel in Grand Junction on August 4:
Our Forest, Our Water, Our Land: Local Impacts on Climate Change. Sponsored by Conservation Colorado, Mesa County Library, Math & Science Center
On the possibility of through passage of asteroid bodies across the Earth’s a...Sérgio Sacani
We have studied the conditions of through passage of asteroids with diameters 200, 100, and
50 m, consisting of three types of materials – iron, stone, and water ice, across the Earth’s
atmosphere with a minimum trajectory altitude in the range 10–15 km. The conditions of this
passage with a subsequent exit into outer space with the preservation of a substantial fraction
of the initial mass have been found. The results obtained support our idea explaining one of the
long-standing problems of astronomy – the Tunguska phenomenon, which has not received
reasonable and comprehensive interpretations to date. We argue that the Tunguska event was
caused by an iron asteroid body, which passed through the Earth’s atmosphere and continued
to the near-solar orbit.
High-resolution UV/Optical/IR Imaging of Jupiter in 2016–2019Sérgio Sacani
Imaging observations of Jupiter with high spatial resolution were acquired beginning in 2016, with a cadence of 53
days to coincide with atmospheric observations of the Juno spacecraft during each perijove pass. The Wide Field
Camera 3 (WFC3) aboard the Hubble Space Telescope (HST) collected Jupiter images from 236 to 925 nm in 14
filters. The Near-Infrared Imager (NIRI) at Gemini North imaged Jovian thermal emission using a lucky-imaging
approach (co-adding the sharpest frames taken from a sequence of short exposures), using the M′ filter at 4.7 μm.
We discuss the data acquisition and processing and an archive collection that contains the processed WFC3 and
NIRI data (doi:10.17909/T94T1H). Zonal winds remain steady over time at most latitudes, but significant
evolution of the wind profile near 24°N in 2016 and near 15°S in 2017 was linked with convective superstorm
eruptions. Persistent mesoscale waves were seen throughout the 2016–2019 period. We link groups of lightning
flashes observed by the Juno team with water clouds in a large convective plume near 15°S and in cyclones near
35°N–55°N. Thermal infrared maps at the 10.8 micron wavelength obtained at the Very Large Telescope show
consistent high brightness temperature anomalies, despite a diversity of aerosol properties seen in the HST data.
Both WFC3 and NIRI imaging reveal depleted aerosols consistent with downwelling around the periphery of the
15°S storm, which was also observed by the Atacama Large Millimeter/submillimeter Array. NIRI imaging of
the Great Red Spot shows that locally reduced cloud opacity is responsible for dark features within the vortex. The
HST data maps multiple concentric polar hoods of high-latitude hazes.
Artigo descreve como os cientistas utilizaram o Telescópio Espacial Hubble para descobrir a estratosfera num exoplaneta classificado como um Júpiter quente. Descoberta essa que pode ajudar a descobrir como os exoplanetas se formam e qual a composição de suas atmosferas.
SPECTROSCOPIC CONFIRMATION OF THE EXISTENCE OF LARGE, DIFFUSE GALAXIES IN THE...Sérgio Sacani
We recently identified a population of low surface brightness objects in the field of the z = 0.023 Coma cluster,
using the Dragonfly Telephoto Array. Here we present Keck spectroscopy of one of the largest of these “ultradiffuse
galaxies” (UDGs), confirming that it is a member of the cluster. The galaxy has prominent absorption
features, including the Ca II H+K lines and the G-band, and no detected emission lines. Its radial velocity of
cz=6280±120 km s−1 is within the 1σ velocity dispersion of the Coma cluster. The galaxy has an effective
radius of 4.3 ± 0.3 kpc and a Sérsic index of 0.89 ± 0.06, as measured from Keck imaging. We find no indications
of tidal tails or other distortions, at least out to a radius of ∼2re. We show that UDGs are located in a previously
sparsely populated region of the size—magnitude plane of quiescent stellar systems, as they are ∼6 mag fainter
than normal early-type galaxies of the same size. It appears that the luminosity distribution of large quiescent
galaxies is not continuous, although this could largely be due to selection effects. Dynamical measurements are
needed to determine whether the dark matter halos of UDGs are similar to those of galaxies with the same
luminosity or to those of galaxies with the same size.
The importance of comets for the origin of life on Earth has been advocated for many decades. Amino acids are
key ingredients in chemistry, leading to life as we know it. Many primitive meteorites contain amino acids, and it
is generally believed that these are formed by aqueous alterations. In the collector aerogel and foil samples of the
Stardust mission after the flyby at comet Wild 2, the simplest form of amino acids, glycine, has been found
together with precursor molecules methylamine and ethylamine. Because of contamination issues of the samples,
a cometary origin was deduced from the 13C isotopic signature. We report the presence of volatile glycine
accompanied by methylamine and ethylamine in the coma of 67P/Churyumov-Gerasimenko measured by
the ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) mass spectrometer, confirming the
Stardust results. Together with the detection of phosphorus and a multitude of organic molecules, this result
demonstrates that comets could have played a crucial role in the emergence of life on Earth.
Evidence for the_thermal_sunyaev-zeldovich_effect_associated_with_quasar_feed...Sérgio Sacani
Using a radio-quiet subsample of the Sloan Digital Sky Survey spectroscopic quasar
catalogue, spanning redshifts 0.5–3.5, we derive the mean millimetre and far-infrared
quasar spectral energy distributions (SEDs) via a stacking analysis of Atacama Cosmology
Telescope and Herschel-Spectral and Photometric Imaging REceiver data. We
constrain the form of the far-infrared emission and find 3σ–4σ evidence for the thermal
Sunyaev-Zel’dovich (SZ) effect, characteristic of a hot ionized gas component with
thermal energy (6.2 ± 1.7) × 1060 erg. This amount of thermal energy is greater than
expected assuming only hot gas in virial equilibrium with the dark matter haloes of
(1 − 5) × 1012h
−1M that these systems are expected to occupy, though the highest
quasar mass estimates found in the literature could explain a large fraction of this
energy. Our measurements are consistent with quasars depositing up to (14.5±3.3) τ
−1
8
per cent of their radiative energy into their circumgalactic environment if their typical
period of quasar activity is τ8 × 108 yr. For high quasar host masses, ∼ 1013h
−1M,
this percentage will be reduced. Furthermore, the uncertainty on this percentage is
only statistical and additional systematic uncertainties enter at the 40 per cent level.
The SEDs are dust dominated in all bands and we consider various models for dust
emission. While sufficiently complex dust models can obviate the SZ effect, the SZ
interpretation remains favoured at the 3σ–4σ level for most models.
WHERE IS THE FLUX GOING? THE LONG-TERM PHOTOMETRIC VARIABILITY OF BOYAJIAN’S ...Sérgio Sacani
We present ∼ 800 days of photometric monitoring of Boyajian’s Star (KIC 8462852) from the AllSky
Automated Survey for Supernovae (ASAS-SN) and ∼ 4000 days of monitoring from the All Sky
Automated Survey (ASAS). We show that from 2015 to the present the brightness of Boyajian’s Star
has steadily decreased at a rate of 6.3 ± 1.4 mmag yr−1
, such that the star is now 1.5% fainter than it
was in February 2015. Moreover, the longer time baseline afforded by ASAS suggests that Boyajian’s
Star has also undergone two brightening episodes in the past 11 years, rather than only exhibiting a
monotonic decline. We analyze a sample of ∼ 1000 comparison stars of similar brightness located in
the same ASAS-SN field and demonstrate that the recent fading is significant at & 99.4% confidence.
The 2015 − 2017 dimming rate is consistent with that measured with Kepler data for the time period
from 2009 to 2013. This long-term variability is difficult to explain with any of the physical models
for the star’s behavior proposed to date
A brief report on the interesting and exotic atmospheric phenomenon observed on extraterrestrial planets. this report is intended to go hand-in-hand with the presentation previous uploaded
TEMPORAL EVOLUTION OF THE HIGH-ENERGY IRRADIATION AND WATER CONTENT OF TRAPPI...Sérgio Sacani
The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting planets, some of which could
harbour liquid water on their surfaces. UV observations are essential to measure their high-energy
irradiation, and to search for photodissociated water escaping from their putative atmospheres. Our
new observations of TRAPPIST-1 Ly-α line during the transit of TRAPPIST-1c show an evolution of
the star emission over three months, preventing us from assessing the presence of an extended hydrogen
exosphere. Based on the current knowledge of the stellar irradiation, we investigated the likely history
of water loss in the system. Planets b to d might still be in a runaway phase, and planets within the
orbit of TRAPPIST-1g could have lost more than 20 Earth oceans after 8 Gyr of hydrodynamic escape.
However, TRAPPIST-1e to h might have lost less than 3 Earth oceans if hydrodynamic escape stopped
once they entered the habitable zone. We caution that these estimates remain limited by the large
uncertainty on the planet masses. They likely represent upper limits on the actual water loss because
our assumptions maximize the XUV-driven escape, while photodissociation in the upper atmospheres
should be the limiting process. Late-stage outgassing could also have contributed significant amounts
of water for the outer, more massive planets after they entered the habitable zone. While our results
suggest that the outer planets are the best candidates to search for water with the JWST, they also
highlight the need for theoretical studies and complementary observations in all wavelength domains
to determine the nature of the TRAPPIST-1 planets, and their potential habitability.
Keywords: planetary systems - Stars: individual: TRAPPIST-1
Very regular high-frequency pulsation modes in young intermediate-mass starsSérgio Sacani
Asteroseismology probes the internal structures of stars by using their natural
pulsation frequencies1. It relies on identifying sequences of pulsation modes that can
be compared with theoretical models, which has been done successfully for many
classes of pulsators, including low-mass solar-type stars2, red giants3, high-mass stars4
and white dwarfs5. However, a large group of pulsating stars of intermediate mass—the
so-called δ Scuti stars—have rich pulsation spectra for which systematic mode
identification has not hitherto been possible6,7. This arises because only a seemingly
random subset of possible modes are excited and because rapid rotation tends to
spoil regular patterns8–10. Here we report the detection of remarkably regular
sequences of high-frequency pulsation modes in 60 intermediate-mass
main-sequence stars, which enables definitive mode identification. The space
motions of some of these stars indicate that they are members of known associations
of young stars, as confirmed by modelling of their pulsation spectra.
EXTINCTION AND THE DIMMING OF KIC 8462852Sérgio Sacani
To test alternative hypotheses for the behavior of KIC 8462852, we obtained measurements of the star
over a wide wavelength range from the UV to the mid-infrared from October 2015 through December
2016, using Swift, Spitzer and at AstroLAB IRIS. The star faded in a manner similar to the longterm
fading seen in Kepler data about 1400 days previously. The dimming rate for the entire period
reported is 22.1 ± 9.7 milli-mag yr−1
in the Swift wavebands, with amounts of 21.0 ± 4.5 mmag in
the groundbased B measurements, 14.0 ± 4.5 mmag in V , and 13.0 ± 4.5 in R, and a rate of 5.0 ± 1.2
mmag yr−1 averaged over the two warm Spitzer bands. Although the dimming is small, it is seen at
& 3 σ by three different observatories operating from the UV to the IR. The presence of long-term
secular dimming means that previous SED models of the star based on photometric measurements
taken years apart may not be accurate. We find that stellar models with Tef f = 7000 - 7100 K and
AV ∼ 0.73 best fit the Swift data from UV to optical. These models also show no excess in the
near-simultaneous Spitzer photometry at 3.6 and 4.5 µm, although a longer wavelength excess from
a substantial debris disk is still possible (e.g., as around Fomalhaut). The wavelength dependence of
the fading favors a relatively neutral color (i.e., RV & 5, but not flat across all the bands) compared
with the extinction law for the general ISM (RV = 3.1), suggesting that the dimming arises from
circumstellar material
The future life span of Earth’s oxygenated atmosphereSérgio Sacani
Earth’s modern atmosphere is highly oxygenated and is a remotely detectable signal of
its surface biosphere. However, the lifespan of oxygen-based biosignatures in Earth’s
atmosphere remains uncertain, particularly for the distant future. Here we use a
combined biogeochemistry and climate model to examine the likely timescale of
oxygen-rich atmospheric conditions on Earth. Using a stochastic approach, we find that
the mean future lifespan of Earth’s atmosphere, with oxygen levels more than 1% of the
present atmospheric level, is 1.08 ± 0.14 billion years (1σ). The model projects that a
deoxygenation of the atmosphere, with atmospheric O2 dropping sharply to levels
reminiscent of the Archaean Earth, will most probably be triggered before the inception
of moist greenhouse conditions in Earth’s climate system and before the extensive loss
of surface water from the atmosphere. We find that future deoxygenation is an
inevitable consequence of increasing solar fluxes, whereas its precise timing is
modulated by the exchange flux of reducing power between the mantle and the ocean–
atmosphere–crust system. Our results suggest that the planetary carbonate–silicate cycle
will tend to lead to terminally CO2-limited biospheres and rapid atmospheric
deoxygenation, emphasizing the need for robust atmospheric biosignatures applicable
to weakly oxygenated and anoxic exoplanet atmospheres and highlighting the potential
importance of atmospheric organic haze during the terminal stages of planetary
habitability.
From our climate panel in Grand Junction on August 4:
Our Forest, Our Water, Our Land: Local Impacts on Climate Change. Sponsored by Conservation Colorado, Mesa County Library, Math & Science Center
First results from_the_hubble_opal_program_jupiter_in_2015Sérgio Sacani
Os cientistas usando o Telescópio Espacial Hubble da NASA/ESA produziram novos mapas de Júpiter, que mostram as contínuas mudanças que ocorrem com a famosa Grande Mancha Vermelha. As imagens também revelam uma rara estrutura em forma de onda na atmosfera do planeta que não tinha sido vista por décadas. A nova imagem é a primeira de uma série de retratos anuais dos planetas externos do Sistema Solar, que nos darão um novo olhar desses mundos remotos, e ajudarão os cientistas a estudarem como eles mudam com o passar do tempo.
Nessa nova imagem de Júpiter, uma grande quantidade de feições foi capturada incluindo ventos, nuvens e tempestades. Os cientistas por trás dessas novas imagens, as obtiveram usando a Wide Field Camera 3 do Hubble, num período de observação de mais de 10 horas e produziram assim dois mapas completos do planeta, a partir das suas observações. Esses mapas fizeram com que fosse possível determinar a velocidade dos ventos em Júpiter, com a finalidade de identificar diferentes fenômenos na sua atmosfera além de traquear as suas feições mais famosas.
As novas imagens confirmam que a grande tempestade que tem existido na superfície de nuvens de Júpiter por no mínimo 300 anos, continua a encolher, mas mesmo que desapareça, ela irá morrer lutando. A tempestade, conhecida como Grande Mancha Vermelha, é vista aqui fazendo seus movimentos em espiral no centro da imagem do planeta. Ela tem diminuído de tamanho de maneira muito rápida de ano em ano. Mas agora, a taxa de encolhimento parece ter reduzido novamente, mesmo apesar da mancha ser cerca de 240 quilômetros menor do que era em 2014.
Analysis of Stratospheric Tropospheric Intrusion as a Function of Potential V...Kalaivanan Murthy
This work is done as a part of a graduate course on Global Air Pollutants in April 2016. The author was pursuing MS in Environmental Engineering Sciences at the University of Florida during the making of this project.
Kim Cobb's Borneo stalagmite talk - AGU 2015Kim Cobb
This talk presents the latest results from the Borneo stalagmite project that seeks to reconstruct Western tropical Pacific hydrology over the last half million years. We discuss our results in the context of climate forcing, the El Nino-Southern Oscillation, and climate modeling studies.
Richard's aventures in two entangled wonderlandsRichard Gill
Since the loophole-free Bell experiments of 2020 and the Nobel prizes in physics of 2022, critics of Bell's work have retreated to the fortress of super-determinism. Now, super-determinism is a derogatory word - it just means "determinism". Palmer, Hance and Hossenfelder argue that quantum mechanics and determinism are not incompatible, using a sophisticated mathematical construction based on a subtle thinning of allowed states and measurements in quantum mechanics, such that what is left appears to make Bell's argument fail, without altering the empirical predictions of quantum mechanics. I think however that it is a smoke screen, and the slogan "lost in math" comes to my mind. I will discuss some other recent disproofs of Bell's theorem using the language of causality based on causal graphs. Causal thinking is also central to law and justice. I will mention surprising connections to my work on serial killer nurse cases, in particular the Dutch case of Lucia de Berk and the current UK case of Lucy Letby.
This pdf is about the Schizophrenia.
For more details visit on YouTube; @SELF-EXPLANATORY;
https://www.youtube.com/channel/UCAiarMZDNhe1A3Rnpr_WkzA/videos
Thanks...!
Introduction:
RNA interference (RNAi) or Post-Transcriptional Gene Silencing (PTGS) is an important biological process for modulating eukaryotic gene expression.
It is highly conserved process of posttranscriptional gene silencing by which double stranded RNA (dsRNA) causes sequence-specific degradation of mRNA sequences.
dsRNA-induced gene silencing (RNAi) is reported in a wide range of eukaryotes ranging from worms, insects, mammals and plants.
This process mediates resistance to both endogenous parasitic and exogenous pathogenic nucleic acids, and regulates the expression of protein-coding genes.
What are small ncRNAs?
micro RNA (miRNA)
short interfering RNA (siRNA)
Properties of small non-coding RNA:
Involved in silencing mRNA transcripts.
Called “small” because they are usually only about 21-24 nucleotides long.
Synthesized by first cutting up longer precursor sequences (like the 61nt one that Lee discovered).
Silence an mRNA by base pairing with some sequence on the mRNA.
Discovery of siRNA?
The first small RNA:
In 1993 Rosalind Lee (Victor Ambros lab) was studying a non- coding gene in C. elegans, lin-4, that was involved in silencing of another gene, lin-14, at the appropriate time in the
development of the worm C. elegans.
Two small transcripts of lin-4 (22nt and 61nt) were found to be complementary to a sequence in the 3' UTR of lin-14.
Because lin-4 encoded no protein, she deduced that it must be these transcripts that are causing the silencing by RNA-RNA interactions.
Types of RNAi ( non coding RNA)
MiRNA
Length (23-25 nt)
Trans acting
Binds with target MRNA in mismatch
Translation inhibition
Si RNA
Length 21 nt.
Cis acting
Bind with target Mrna in perfect complementary sequence
Piwi-RNA
Length ; 25 to 36 nt.
Expressed in Germ Cells
Regulates trnasposomes activity
MECHANISM OF RNAI:
First the double-stranded RNA teams up with a protein complex named Dicer, which cuts the long RNA into short pieces.
Then another protein complex called RISC (RNA-induced silencing complex) discards one of the two RNA strands.
The RISC-docked, single-stranded RNA then pairs with the homologous mRNA and destroys it.
THE RISC COMPLEX:
RISC is large(>500kD) RNA multi- protein Binding complex which triggers MRNA degradation in response to MRNA
Unwinding of double stranded Si RNA by ATP independent Helicase
Active component of RISC is Ago proteins( ENDONUCLEASE) which cleave target MRNA.
DICER: endonuclease (RNase Family III)
Argonaute: Central Component of the RNA-Induced Silencing Complex (RISC)
One strand of the dsRNA produced by Dicer is retained in the RISC complex in association with Argonaute
ARGONAUTE PROTEIN :
1.PAZ(PIWI/Argonaute/ Zwille)- Recognition of target MRNA
2.PIWI (p-element induced wimpy Testis)- breaks Phosphodiester bond of mRNA.)RNAse H activity.
MiRNA:
The Double-stranded RNAs are naturally produced in eukaryotic cells during development, and they have a key role in regulating gene expression .
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
Seminar of U.V. Spectroscopy by SAMIR PANDASAMIR PANDA
Spectroscopy is a branch of science dealing the study of interaction of electromagnetic radiation with matter.
Ultraviolet-visible spectroscopy refers to absorption spectroscopy or reflect spectroscopy in the UV-VIS spectral region.
Ultraviolet-visible spectroscopy is an analytical method that can measure the amount of light received by the analyte.
1. deliver westward acceleration to the mean flow.
Furthermore, the stronger tropical upwelling dur-
ing Boreal winter slows down the QBO’s descent,
allowing more time for the extratropical waves to
impact during this particular phase.
Of course, it is also possible that our current
numerical models can not properly represent the
processes disrupting the QBO. To investigate
this, the foregoing RMS analysis that was applied
to the observational record was applied to his-
torical global climate model runs so as to identify
possible analogous events (Fig. 4, A to C). Among
the available models that produce a QBO inter-
nally, only one rarely produced behavior similar
totheobserveddisruption, withanexampleshown
in Fig. 4D. The extreme profiles resemble those
observed during 2016 with a thin layer of west-
ward wind appearing within an otherwise east-
ward QBO phase.
What will happen next? The recent disruption
of the QBO is a rare event that occurs in the
northern winter. The forecast initialized after
the disruption (Fig. 3B) suggests that the QBO
will return to more regular phase progression
over the coming year. The westward jet that
suddenly appeared in the lower stratosphere is
predicted to amplify in the summer of 2016 and
progress downward with time. Eastward flow then
descends from the 20-hPa level and dominates
the lower stratospheric flow toward the end of
2016, returning the QBO to its typical behavior.
We then expect regular and predictable QBO
cycling to continue from 2017, as occurs in the
available climate models (Fig. 4D). Nonetheless,
as the climate warms in the future, climate models
that simulate these events suggest that similar dis-
ruptions will occur up to three times every 100 years
for the more extreme of the standard climate
change scenarios. This is consistent with a pro-
jected strengthening of the Brewer-Dobson cir-
culation due to increasing stratospheric wave
activity (14) and the recently observed weakening
of the QBO amplitude in the lower stratosphere
(21) under climate change. However, robustly
modeling how the QBO and its underlying pro-
cesses and external influences will change in
the future remains elusive.
There is a further outcome of the 2016 dis-
ruption of the QBO. After an eastward QBO at
the onset of the 2015–2016 winter, the QBO at the
onset of the coming winter of 2016–2017 was
expected to be westward. The disruption of early
2016 means that an eastward QBO phase is now
again expected in the lower stratosphere. Because
of the expected QBO influence on the Atlantic jet
stream, this increases the risk of a strong jet,
winter storms, and heavy rainfall over northern
Europe in the coming winter (22, 23).
Note added in proof: A similar finding was pub-
lished by Newman et al. (24) during the final re-
vision period of the present study.
REFERENCES AND NOTES
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8. J. A. Anstey, T. G. Shepherd, Q. J. R. Meteorol. Soc. 140, 1–21
(2014).
9. J. Kidston et al., Nat. Geosci. 8, 433–440 (2015).
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11. B. Naujokat, J. Atmos. Sci. 43, 1873–1877 (1986).
12. R. S. Lindzen, J. R. Holton, J. Atmos. Sci. 25, 1095–1107 (1968).
13. J. R. Holton, R. S. Lindzen, J. Atmos. Sci. 29, 1076–1080(1972).
14. N. Butchart, Rev. Geophys. 52, 157–184 (2014).
15. A. R. Plumb, R. C. Bell, Q. J. R. Meteorol. Soc. 108, 335–352
(1982).
16. R. E. Dickinson, J. Atmos. Sci. 25, 984–1002 (1968).
17. T. J. Dunkerton, Atmos.-Ocean 21, 55–68 (1983).
18. K. Hamilton, A. Hertzog, F. Vial, G. Stenchikov, J. Atmos. Sci.
61, 383–402 (2004).
19. J. S. Kinnersley, S. Pawson, J. Atmos. Sci. 53, 1937–1949 (1996).
20. C. MacLachlan et al., Q. J. R. Meteorol. Soc. 141, 1072–1084
(2015).
21. Y. Kawatani, K. Hamilton, Nature 497, 478–481 (2013).
22. R. A. Ebdon, Aust. Meteorol. Mag. 104, 282–285 (1975).
23. C. Huntingford et al., Nat. Clim. Change 4, 769–777 (2014).
24. P. A. Newman, L. Coy, S. Pawson, L. R. Lait, Geophys. Res. Lett.
10.1002/2016GL070373 (2016).
25. D. P. Dee et al., Q. J. R. Meteorol. Soc. 137, 553–597 (2011).
26. D. G. Andrews, M. E. McIntyre, J. Atmos. Sci. 33, 2031–2048
(1976).
27. NCAS British Atmospheric Data Centre, European Centre for
Medium-Range Weather Forecasts: ECMWF operational
analysis: Assimilated Data (2006); http://catalogue.ceda.ac.
uk/uuid/c46248046f6ce34fc7660a36d9b10a71.
28. E. P. Gerber et al., Bull. Am. Meteorol. Soc. 93, 845–859 (2012).
ACKNOWLEDGMENTS
We thank the European Centre for Medium-Range Weather
Forecasts for providing ERA-Interim and Operational Analysis data
(www.ecmwf.int/en/forecasts) and the Freie Universität Berlin for
providing radiosonde data (www.geo.fu-berlin.de/en/met/ag/
strat/produkte/qbo). The CMIP5 data was obtained from the
British Atmospheric Data Centre (browse.ceda.ac.uk/browse/
badc/cmip5). A summary of data used in the study is listed in
table S1. S.M.O. was supported by UK Natural Environment Research
Council grants NE/M005828/1 and NE/P006779/1. A.A.S., J.R.K.,
and N.B. were supported by the Joint UK Business, Energy and
Industrial Strategy/Defra Met Office Hadley Centre Climate
Programme (GA01101). A.A.S. and J.R.K. were additionally supported
by the EU Seventh Framework Programme SPECS (Seasonal-to-
decadal climate Prediction for the improvement of European Climate
Services) project. We acknowledge the scientific guidance of the
World Climate Research Programme for helping motivate this work,
coordinated under the framework of the Stratosphere-troposphere
Processes and their Role in Climate (SPARC) QBOi activity led by
S.M.O., J.A.A., N.B., and K.H. The analysis of observations and
reanalyses was performed by K.H., C.Z., S.M.O., J.A.A., and N.B.
J.R.K. and A.A.S. provided the analysis of the seasonal forecasts, and
V.S. identified analogous events in global climate model output.
A.A.S. first alerted us to the disruption of the QBO in observational
data. All authors were equally involved in the interpretation of the
results and preparation of the manuscript.
SUPPLEMENTARY MATERIALS
www.sciencemag.org/content/353/6306/1424/suppl/DC1
Table S1
2 July 2016; accepted 29 August 2016
10.1126/science.aah4156
ATMOSPHERIC OXYGEN
A Pleistocene ice core record of
atmospheric O2 concentrations
D. A. Stolper,1
* M. L. Bender,1,2
G. B. Dreyfus,1,3
† Y. Yan,1
J. A. Higgins1
The history of atmospheric O2 partial pressures (PO2) is inextricably linked to the
coevolution of life and Earth’s biogeochemical cycles. Reconstructions of past PO2
rely on models and proxies but often markedly disagree. We present a record of PO2
reconstructed using O2/N2 ratios from ancient air trapped in ice. This record
indicates that PO2 declined by 7 per mil (0.7%) over the past 800,000 years, requiring
that O2 sinks were ~2% larger than sources. This decline is consistent with changes
in burial and weathering fluxes of organic carbon and pyrite driven by either
Neogene cooling or increasing Pleistocene erosion rates. The 800,000-year record of
steady average carbon dioxide partial pressures (PCO2) but declining PO2 provides
distinctive evidence that a silicate weathering feedback stabilizes PCO2 on million-year
time scales.
T
he importance of O2 to biological and geo-
chemical processes has led to a long-standing
interest in reconstructing past atmospheric
O2 partial pressures (PO2, reported at stan-
dard temperature and pressure) (1–12). How-
ever, there is no consensus on the history of
Phanerozoic PO2, with reconstructions disagree-
ing by as much as 0.2 atm, the present-day pres-
sure of O2 in the atmosphere (e.g., 7, 10). Even
over the past million years, it is not known whether
atmospheric O2 concentrations varied or whether
the O2 cycle was in steady state (Fig. 1A). Knowl-
edge of PO2 over the past million years could
provide new insights into the O2 cycle on geologic
time scales and serve as a test for models and
proxies of past PO2. Here we present a primary
record of PO2 over the past 800,000 years, recon-
structed using measured O2/N2 ratios of ancient air
trapped in polar ice.
O2/N2 ratios of this kind have been extensively
used to date ice cores on the basis of the corre-
lation between O2/N2 and local summertime
SCIENCE sciencemag.org 23 SEPTEMBER 2016 • VOL 353 ISSUE 6306 1427
1
Department of Geosciences, Princeton University, Princeton,
NJ 08544, USA. 2
Institute of Oceanology, Shanghai Jiao Tong
University, Shanghai 200240, China. 3
Laboratoire des Sciences
du Climat et de l'Environnement, Gif-sur-Yvettte, France.
*Corresponding author. Email: dstolper@princeton.edu
†Present address: U.S. Department of Energy, Washington, DC
20585, USA.
RESEARCH | REPORTS
onSeptember22,2016http://science.sciencemag.org/Downloadedfrom
2. insolation (13–17). Despite being directly tied to
atmosphericcompositions,O2/N2 ratioshavenever
before been used to reconstruct past PO2. Landais
et al. (16) and Bazin et al. (17), while using O2/N2
ratios for ice core dating, noted a decline in O2/N2
values with time (i.e., toward the present). They
suggested that this decline could be due to sec-
ular changes in air entrapment processes, gas
loss during core storage, or changes in atmospheric
O2/N2, but they did not evaluate these hypotheses.
Given the potential for O2/N2 ratios to directly
constrain Pleistocene PO2, we present compiled
O2/N2 measurements from multiple ice core re-
cords and evaluate their geochemical implications.
We compiled published O2/N2 ice core records
from Greenland [Greenland Ice Sheet Project 2
(GISP2) (18)] and Antarctica [Vostok (13), Dome
F (14), and Dome C (17); table S1], along with
previously unpublished Antarctic Ar/N2 records
[Vostok and Dome C; table S2]. The data were
treated as follows [see (19) for more details]. (i)
Measured ratios were corrected for gravitational
fractionations and are reported using d notation
dO2=N2 ¼ 1000Â
½O2Š=½N2Šsample
½O2Š=½N2Špreanthropogenic atmosphere
−1
!
ð1Þ
dAr=N2 ¼ 1000Â
½ArŠ=½N2Šsample
½ArŠ=½N2Šmodern atmosphere
−1
!
ð2Þ
where brackets denote concentrations. A decrease
indO2/N2 of1permil(‰)equatestoa0.1%decrease
in PO2 relative to the preanthropogenic atmosphere
(i.e., the modern atmosphere corrected for fossil
fuel combustion). We define the preanthropogenic
atmosphere as having dO2/N2 = 0‰ and dAr/N2 =
0‰. (ii) Only analyses of bubble-free ice with
clathrates were considered. (iii) The portions of
the dO2/N2 and dAr/N2 signals linked to insola-
tion (13–17) were removed (figs. S1 and S2). (iv)
We corrected for differences in bubble close-off
fractionations between ice cores and interlabo-
ratory offsets by assuming that, in the absence of
such effects, trapped gases of a given age share
identical atmospheric O2/N2 and Ar/N2 values
(figs. S3 and S4).
The fully corrected data are plotted versus ice
age in Figs. 1B (dO2/N2) and 2A (dAr/N2). dΟ2/N2
values decrease by 8.4‰ per million years (±0.2,
1s), consistent with the observations of Landais
et al. (16) and Bazin et al. (17). dAr/N2 values in-
crease by 1.6‰ per million years (±0.2, 1s), which
is discussed below.
The decline in dO2/N2 with time could result
from temporal changes in bubble entrapment
processes, effects of ice core storage, a decline in
PO2, or an increase in the partial pressure of atmo-
spheric N2 (PN2). We now evaluate these possi-
bilities in the context of the dO2/N2 record.
dO2/N2 values of gas extracted from ice are ~5
to10‰lowerthanthoseofambientair(13–18,20,21).
Additionally, dAr/N2 covaries with dO2/N2 along
slopes of 0.3 to 0.6 (fig. S5) (19, 21, 22). These
depletions and covariations have been attributed
to fractionations created during bubble close-off
on the basis of measurements and models of firn
air (20, 22) and the covariation of dO2/N2 and
dAr/N2 with local insolation (figs. S1 and S2)
(13–17, 19). If secular changes in bubble close-off
fractionations caused the decline in dO2/N2, then
dAr/N2 values should covary with dO2/N2 along
slopes of 0.3 to 0.6 and thus decline by 2.5 to 5.0‰
per million years. Instead, dAr/N2 increases with
time by 1.6‰ per million years (±0.2, 1s; Fig. 2A).
The increasing trend is largely due to a subset of
Vostok data from 330,000- to 370,000-year-old ice
that is lower in dAr/N2 by ~1‰ compared with
younger data. Exclusion of this subset yields an
increase in dAr/N2 with time of only 0.35‰ (±0.20,
1s), within the 2s error range of no change. Re-
gardless, whichever way the dAr/N2 are ana-
lyzed, they are inconsistent with the decline in
dO2/N2 being caused by bubble close-off pro-
cesses (Fig. 2A).
Ice core storage, under some conditions, causes
the dO2/N2 values of trapped gases to decline
(14–17). Thus, the second possibility that we con-
sider is that ice core storage lowered the dO2/N2
values so that the slope observed in Fig. 1 is an
artifact. For example, a change in dO2/N2 cor-
related with ice age but unrelated to atmospheric
compositions could result if the retention of O2
versus N2 during storage is a function of pre-
coring properties controlled by original ice depths
(e.g., in situ temperature, pressure, or clathrate
size). We evaluate this possibility by using three
approaches. (i) Gas loss during core storage causes
dAr/N2 todeclineathalftherateofdO2/N2 (21,23,24).
However, as discussed above, the dAr/N2 values
are not consistent with such a change (Fig. 2A).
(ii) Because some ice properties (e.g., temperature
and pressure) can vary linearly with ice depth,
we tested whether the Dome C dO2/N2 data are
better fit by a linear relationship when plotted
against ice age or depth. We note that only the
Dome C ice core’s age-depth relationship is suffi-
ciently curvilinear for this test to be useful. We
linearly regressed both age and depth against
1428 23 SEPTEMBER 2016 • VOL 353 ISSUE 6306 sciencemag.org SCIENCE
O2/N2(‰)
age (kyr)age (kyr)
-4
-2
0
2
4
6
8
10
-4
-2
0
2
4
6
8
10
0 600400200 800
Dome F
Vostok
Dome C
Best-fit line:
Slope = 8.4 ‰/myr (±0.2, 1 )
20.95
21.03
21.12
20.87
PO2(100xatm)
GISP2
-15
-10
-5
0
5
10
15
20
25
30
0 200 400 600 800000 200200200 400400400 600600600 800800800
Glasspool and Scott (2010) [11]
Falkowski et al. (2005) [7]
ice core data
best-fit line
Kump and Garrels (1986) [1]
Shackleton (1987) [2]
Berner and Canfield (1989) [3]
Derry and France-Lanord (1996) [4]
Tappert et al. (2013) [12]
Hansen and Wallmann (2003) [5]
Bergman et al. (2004) [6]
Arvidson et al. (2006) [8]
Berner (2006) [9]
Berner (2009) [10]
20.95
21.16
21.37
20.74
PO2(100xatm)
21.58
O2/N2(‰)
[2]
[9]
[7]
[6]
best-fit
line
[1]
[11]
[5]
[4]
[12]
[3]
[8]
[10]
Fig. 1. dO2/N2 and PO2 values versus age from ice cores and from model and proxy predictions. (A) Comparison of the ice core data with model and
proxy predictions (1–12). (B) dO2/N2 versus ice age from ice cores. dO2/N2 decreases by 8.4‰ per million years (±0.2, 1s). Gray bands are 95% confidence
intervals. Data are corrected for gravitational, interlaboratory, and bubble close-off fractionations (19). kyr, thousand years; myr, million years.
RESEARCH | REPORTS
onSeptember22,2016http://science.sciencemag.org/Downloadedfrom
3. dO2/N2 for ice older than ~400,000 years (i.e.,
deeper than 2600 m) and extrapolated the fits to
younger ages and shallower depths. The extrap-
olation forage(Fig. 2B)passesthrough the younger
data, whereas the extrapolation for depth (Fig. 2C)
misses the shallower data (by >4s). (iii) Repeat
dO2/N2 measurements of Vostok ice from the same
age interval (150,000 to 450,000 years ago) made
10 years apart (13, 15) differ onaverage by 6‰, with
longer storage leading to lower dO2/N2. Despite
this, regressing dO2/N2 against time yields statisti-
cally identical (within 1s) slopes of dO2/N2 versus
age for both data sets (fig. S6).
Collectively, the data and tests presented above
provide no support for the observed decrease in
dO2/N2 over time being an artifact of either bubble
close-off processes as they are currently under-
stood or ice core storage. Consequently, we hy-
pothesize and proceed with the interpretation
that the observed decline in dO2/N2 reflects changes
in PO2 or PN2. Because N2 has a billion-year at-
mosphericlifetime(25),welinkthedeclineindO2/N2
with time exclusively to a decline in PO2. Our
hypothesis is further supported by the observa-
tion that data from all four ice cores individually
exhibit the same general trends and magnitudes
of decreasing dO2/N2 with time (table S3), even
though each was drilled, stored, and analyzed
differently.
The question raised by this record is why PO2
has decreased by ~7‰ over the past 800,000 years.
Changes in PO2 require imbalances between
O2 sources [dominantly modern sedimentary
organic carbon (Corg) and pyrite burial] and sinks
(dominantly ancient sedimentary Corg and pyrite
oxidation) (26). Thus, a higher rate of oxidative
weathering relative to Corg and/or pyrite burial
over the past million years could
have caused the observed PO2 de-
cline. The ~2-million-year (+1.5/
–0.5 million years) (26) geological
residence time of O2, combined
with the decline in dO2/N2 of
8.4‰ per million years, indicates
that O2 sinks were 1.7% larger than
sources over the past 800,000 years
(27). We now explore possible causes
for this drawdown, examining first
the impact of changing erosion rates
and second the impact of global
cooling on PO2.
Global erosion rates influence
the amount of rock weathered (con-
suming O2) and sediment buried
(releasing O2). These rates have
been suggested to have increased
up to 100% in the Pleistocene rel-
ative to the Pliocene (28) [though
this is debated (29)]. Thus, the pos-
sibility exists that increased Pleisto-
cene sedimentary erosion and burial
rates affected PO2 levels. Indeed,
Torres et al. (30) modeled that in-
creasing erosion rates over the past
15 million years enhanced oxida-
tion of sedimentary pyrite rela-
tive to burial so that PO2 declined
on average by 9 to 25‰ per million years. This is
similar to the decline given by the ice core record
(8.4‰ per million years). We note that whether
increasing erosion rates cause PO2 to decline
(instead of increase) is unknown (31).
Large increases (e.g., 100%) in Pleistocene ero-
sion rates, if they did occur, likely would have
required processes that keep O2 sources and sinks
balanced within ~2% (the observed imbalance).
Such processes could include the proposed PO2-
dependent control of Corg burial fluxes on sedimen-
tary phosphorus burial rates (32). Alternatively,
sedimentary mineral surface area is known to
positively correlate with total sedimentary Corg and
pyrite content (33). Hedges and Kiel (33) pro-
posed that the total eroded and total buried min-
eral surface areas today are about equal. If this
was true in the past, the conservation of eroded
versus newly generated mineral surface area may
have acted to balance Corg and pyrite weathering
and burial fluxes (and thus O2 fluxes), regardless of
global erosion rates (33).
Alternatively, on the basis of 13
C/12
C and 18
O/16
O
records from sedimentary carbonates, Shackleton
(2) proposed that PO2 declined over the Neogene as
a result of oceaniccooling. He suggestedthefollowing
feedback loop: Cooling increases O2 solubility. This
raises dissolved O2 concentrations, which increases
the volume of ocean sediment exposed to dissolved
O2 and thus also increases global aerobic Corg
remineralization rates (33). On million-year time
scales, Corg burial rates and, therefore, PO2 and O2
concentrations decline until seawater O2 concen-
trations return to their initial (precooling) levels. At
this new steady state, Corg burial rates have returned
to their original values, but PO2 is stabilized at a
lower value.
Shackleton’s hypothesis can be evaluated to first
order in the context of the dO2/N2 data by using
records of past ocean temperature. Specifically,
temperatures in the deep (>1000 m depth) ocean
were roughly constant from 24 to 14 million years
ago (34, 35). Assuming an O2 residence time of ~2
million years and the hypothesis that changes in
ocean temperature modulate PO2, then O2 sources
and sinks would have been in balance by 14 million
years ago. The oceans have cooled on average by
0.3°C per million years over the past 14 million
years and 0.5° to 1.1°C per million years over the
past 5 million years (34, 35). Cooling of 0.3° to 1.1°C
per million years increases O2 solubility by ~7 to
25‰ per million years (36). If dissolved O2 con-
centrations remained constant (as this hypothesis
requires), such changes in O2 solubility necessitate
a decline in PO2 of ~7 to 25‰ per million years.
These rates bracket the rate of decline given by the
ice core record (8.4‰ per million years; Fig. 1A).
We note that deep ocean cooling rates track aver-
age marine cooling rates, but not precisely, because
modern deep waters form in and thus reflect the
temperatures of high latitudes. Regardless, the
critical point is that this simple calculation is
consistent with the ice core–derived dO2/N2
record and supports the hypothesis that global
temperature stabilizes PO2 on geological time
scales through feedbacks associated with Corg
burial rates.
A drop in PO2 over the past 800,000 years due
solely to changes in Corg burial versus oxidation
rates (regardless of the cause) requires positive
CO2 fluxes (~3 × 1011
moles C per year) into the
ocean and atmosphere (19). However, ice core
records of past carbon dioxide partial pressures
(PCO2) show no obvious change in the mean over
SCIENCE sciencemag.org 23 SEPTEMBER 2016 • VOL 353 ISSUE 6306 1429
age (kyr) age (kyr)
-5-5
00
55
1010
00 200200 400400 600600 800800
-5
0
5
10
0 200 400 600 800
O2/N2, all Ar/N2, Vostok
Ar/N2, Dome C
best-fit
O2/N2 line
Expected range of
Ar/N2 trends if
O2/N2 is controlled
by bubble close-off
fractionations or gas
loss
best-fit
Ar/N2 line
-5
0
5
10
100 450 800
-5-5-5
000
555
101010
100100100 450450450 800800800
-10
-10
-5
0
5
10
1400 2300 3200
depth (m)
-10-10-10
-5-5-5-5
0000
5555
10101010
1400140014001400 2300230023002300 3200320032003200
-5
0
5
10
100 450 800
O2/N2(‰)O2/N2(‰)
(‰)
Fig. 2. Evidence that the observed decline in dO2N2 with time does not originate from either secular changes in
bubble close-off fractionations or ice core storage. (A) dAr/N2 and dO2/N2 versus ice age. Bubble close-off processes
and gas loss would cause dAr/N2 and dO2/N2 to covary with slopes of 0.3 to 0.6. The observed dAr/N2 trend does not
overlap with these expected trends (orange wedge), indicating that such processes did not cause the decline in dO2/N2.
(B) Dome C dO2/N2 versus ice age and (C) versus depth. Dotted lines were fit to ice >400,000 years old or >2600 m deep and
extrapolated to younger ages or shallower depths. Extrapolations of the fits pass through the younger data (B) but miss the
deeper data [beyond 4s (C)], indicating depth-dependent glacial properties did not cause the decline in dO2/N2. Gray bands
are 95% confidence intervals. Data are corrected for gravitational, interlaboratory, and bubble close-off fractionations (19).
RESEARCH | REPORTS
onSeptember22,2016http://science.sciencemag.org/Downloadedfrom
4. the past 800,000 years (37–39) (Fig. 3). To under-
stand how changes in PO2 influence PCO2, we de-
veloped a simple model of the carbon cycle that
allows for changes in weathering and burial rates
of carbonates, Corg, and silicates (19). In the ab-
sence of any PCO2-dependent feedbacks, a constant
decline in dO2/N2 of 8.4‰ over the past million
years from a net imbalance in Corg fluxes causes
PCO2 to rise by ~140 parts per million over the same
time frame. Such a rise is inconsistent with the
PCO2 record (Fig. 3). A PCO2-dependent silicate
weathering feedback (40) can account for the
higher CO2 flux if silicate weathering is enhanced
by ~6% relative to volcanic outgassing. For exam-
ple, response times for silicate weathering of
200,000 to 500,000 years (41) stabilize PCO2 levels
within ~1 million years (Fig. 3).
Changes in Cenozoic climate began millions
of years before the start of our ice core–based
dO2/N2 record 800,000 years ago (e.g., 2, 30, 34, 35).
Thus, we suggest that modest enhancements
in silicate weathering would already have stabi-
lized the portion of the PCO2 ice core record
that is controlled by differences in Corg and
pyrite burial and oxidation. Thus, the combina-
tion of changing PO2 and constant average PCO2
provides distinctive evidence for feedbacks that
regulate PCO2 on geologic time scales (37). Last-
ly, a 2% imbalance in O2 fluxes results in only
a ~0.1‰ shift in the 13
C/12
C ratio of buried
carbon (19).
Our results provide a primary record of declin-
ing PO2 over the past 800,000 years sustained by a
~2% imbalance between O2 sources and sinks.
Critically, this decline is consistent with previously
proposed and relatively simple models that invoke
either the effects of increased Pleistocene erosion
rates or decreased ocean temperature to explain
feedbacks in the global cycles of carbon, sulfur, and
O2—and the effects of both could have contributed
to the observed decline in PO2. Regardless, creat-
ing primary records of past PO2 is the necessary
first step in identifying the fundamental processes
that regulate PO2 on geological time scales. Given
evidence that both global erosion rates and
temperature have changed markedly over the
Cenozoic (42), the ideas presented here may have
implications for the history of PO2 beyond the
Pleistocene.
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ACKNOWLEDGMENTS
D.A.S. acknowledges funding from a National Oceanic and
Atmospheric Administration Climate & Global Change
postdoctoral fellowship. J.A.H. and M.L.B. acknowledge
support from National Science Foundation grant ANT-1443263.
All data presented are available in the supplementary
materials. We thank W. Fischer, I. Halevy, N. Planavsky,
J. Severinghaus, and D. Sigman for helpful discussions and
three anonymous reviewers for helpful comments on the
manuscript. D.A.S., J.A.H., and M.L.B. conceived the study
and wrote the manuscript. D.A.S., J.A.H., M.L.B., and Y.Y.
analyzed the data. G.B.D. measured the Dome C dAr/N2 data.
The views expressed in this article are those of the authors
and do not necessarily represent the views of the Department
of Energy or the U.S. Government.
SUPPLEMENTARY MATERIALS
www.sciencemag.org/content/353/6306/1427/suppl/DC1
Materials and Methods
Figs. S1 to S6
Tables S1 to S3
References (43–78)
25 February 2016; accepted 2 August 2016
10.1126/science.aaf5445
1430 23 SEPTEMBER 2016 • VOL 353 ISSUE 6306 sciencemag.org SCIENCE
Fig. 3. Comparison
of calculated and
measured PCO2
values due to declin-
ing PO2 with and
without a PCO2-
dependent silicate
weathering feed-
back. Inclusion of a
silicate weathering
feedback with geolog-
ically reasonable
response times
[200,000 to 500,000
years (41)] stabilizes
PCO2 within ~1 million
years. Thus, increased
silicate weathering
rates could have
compensated for
enhanced CO2 fluxes
from increased net
Corg oxidation more
than 800,000 years
ago. The PCO2 records
are continuous only
from 800,000 years
to the present. The model used to calculate PCO2 values is described in (19); the measured PCO2
values are from (38) and (39). ppm, parts per million.
150150
200200
250250
300300
350350
400400
00 200200 400400 600600 800800 10001000
150
200
250
300
350
400
0 200 400 600 800 1000
age (kyr)
PCO
2
(ppm)
ice core data
No PCO2-dependent silicate weathering feedback
500-kyr response time for PCO2-dependent silicate weathering feedback
400-kyr response time for PCO2-dependent silicate weathering feedback
300-kyr response time for PCO2-dependent silicate weathering feedback
200-kyr response time for PCO2-dependent silicate weathering feedback
No PCO2-dependent silicate weathering feedback
results in changes in PCO2 inconsistent with measured
ice core records.
A PCO2-dependent silicate weathering feedback stabilizes PCO2 within ~1 million
years following the creation of an imbalance in Corg burial versus weathering rates.
RESEARCH | REPORTS
onSeptember22,2016http://science.sciencemag.org/Downloadedfrom
5. (6306), 1427-1430. [doi: 10.1126/science.aaf5445]353Science
Higgins (September 22, 2016)
D. A. Stolper, M. L. Bender, G. B. Dreyfus, Y. Yan and J. A.
concentrations2A Pleistocene ice core record of atmospheric O
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