The silicate Earth is strongly depleted in moderately volatile
elements (such as lead, zinc, indium and alkali elements) relative
to CI chondrites, the meteorites that compositionally most closely
resemble the Sun1
. This depletion may be explained qualitatively
by accretion of 10 to 20 per cent of a volatile-rich body to a reduced
volatile-free proto-Earth2,3
, followed by partial extraction of some
elements to the core1
. However, there are several unanswered
questions regarding the sources of Earth’s volatiles4,5
, notably the
overabundance of indium in the silicate Earth. Here we examine
the melting processes that occurred during accretion on Earth
and precursor bodies and report vaporization experiments under
conditions of fixed temperature and oxygen fugacity. We find that
the pattern of volatile element depletion in the silicate Earth is
consistent with partial melting and vaporization rather than with
simple accretion of a volatile-rich chondrite-like body. We argue that
melting and vaporization on precursor bodies and possibly during
the giant Moon-forming impact6–8 were responsible for establishing
the observed abundances of moderately volatile elements in Earth.
Synthesis of prebiotic organics from CO2 by catalysis with meteoritic and vo...Sérgio Sacani
The emergence of prebiotic organics was a mandatory step toward the origin of life. The signifcance
of the exogenous delivery versus the in-situ synthesis from atmospheric gases is still under debate.
We experimentally demonstrate that iron-rich meteoritic and volcanic particles activate and catalyse
the fxation of CO2, yielding the key precursors of life-building blocks. This catalysis is robust and
produces selectively aldehydes, alcohols, and hydrocarbons, independent of the redox state of the
environment. It is facilitated by common minerals and tolerates a broad range of the early planetary
conditions (150–300 °C, ≲ 10–50 bar, wet or dry climate). We fnd that up to 6 × 108 kg/year of prebiotic
organics could have been synthesized by this planetary-scale process from the atmospheric CO2 on
Hadean Earth.
Magnesium isotope evidence that accretional vapour loss shapes planetary comp...Sérgio Sacani
It has long been recognized that Earth and other differentiated
planetary bodies are chemically fractionated compared to primitive,
chondritic meteorites and, by inference, the primordial disk
from which they formed. However, it is not known whether the
notable volatile depletions of planetary bodies are a consequence
of accretion1
or inherited from prior nebular fractionation2
. The
isotopic compositions of the main constituents of planetary bodies
can contribute to this debate3–6. Here we develop an analytical
approach that corrects a major cause of measurement inaccuracy
inherent in conventional methods, and show that all differentiated
bodies have isotopically heavier magnesium compositions
than chondritic meteorites. We argue that possible magnesium
isotope fractionation during condensation of the solar nebula,
core formation and silicate differentiation cannot explain these
observations. However, isotopic fractionation between liquid and
vapour, followed by vapour escape during accretionary growth of
planetesimals, generates appropriate residual compositions. Our
modelling implies that the isotopic compositions of magnesium,
silicon and iron, and the relative abundances of the major elements
of Earth and other planetary bodies, are a natural consequence of
substantial (about 40 per cent by mass) vapour loss from growing
planetesimals by this mechanism.
Hydrogen-bearing vesicles in space weathered lunar calcium-phosphatesSérgio Sacani
Water on the surface of the Moon is a potentially vital resource for future lunar bases and
longer-range space exploration. Effective use of the resource depends on developing an
understanding of where and how within the regolith the water is formed and retained. Solar
wind hydrogen, which can form molecular hydrogen, water and/or hydroxyl on the lunar
surface, reacts and is retained differently depending on regolith mineral content, thermal
history, and other variables. Here we present transmission electron microscopy analyses of
Apollo lunar soil 79221 that reveal solar-wind hydrogen concentrated in vesicles as molecular
hydrogen in the calcium-phosphates apatite and merrillite. The location of the vesicles in the
space weathered grain rims offers a clear link between the vesicle contents and solar wind
irradiation, as well as individual grain thermal histories. Hydrogen stored in grain rims is a
source for volatiles released in the exosphere during impacts.
Synthesis of prebiotic organics from CO2 by catalysis with meteoritic and vo...Sérgio Sacani
The emergence of prebiotic organics was a mandatory step toward the origin of life. The signifcance
of the exogenous delivery versus the in-situ synthesis from atmospheric gases is still under debate.
We experimentally demonstrate that iron-rich meteoritic and volcanic particles activate and catalyse
the fxation of CO2, yielding the key precursors of life-building blocks. This catalysis is robust and
produces selectively aldehydes, alcohols, and hydrocarbons, independent of the redox state of the
environment. It is facilitated by common minerals and tolerates a broad range of the early planetary
conditions (150–300 °C, ≲ 10–50 bar, wet or dry climate). We fnd that up to 6 × 108 kg/year of prebiotic
organics could have been synthesized by this planetary-scale process from the atmospheric CO2 on
Hadean Earth.
Magnesium isotope evidence that accretional vapour loss shapes planetary comp...Sérgio Sacani
It has long been recognized that Earth and other differentiated
planetary bodies are chemically fractionated compared to primitive,
chondritic meteorites and, by inference, the primordial disk
from which they formed. However, it is not known whether the
notable volatile depletions of planetary bodies are a consequence
of accretion1
or inherited from prior nebular fractionation2
. The
isotopic compositions of the main constituents of planetary bodies
can contribute to this debate3–6. Here we develop an analytical
approach that corrects a major cause of measurement inaccuracy
inherent in conventional methods, and show that all differentiated
bodies have isotopically heavier magnesium compositions
than chondritic meteorites. We argue that possible magnesium
isotope fractionation during condensation of the solar nebula,
core formation and silicate differentiation cannot explain these
observations. However, isotopic fractionation between liquid and
vapour, followed by vapour escape during accretionary growth of
planetesimals, generates appropriate residual compositions. Our
modelling implies that the isotopic compositions of magnesium,
silicon and iron, and the relative abundances of the major elements
of Earth and other planetary bodies, are a natural consequence of
substantial (about 40 per cent by mass) vapour loss from growing
planetesimals by this mechanism.
Hydrogen-bearing vesicles in space weathered lunar calcium-phosphatesSérgio Sacani
Water on the surface of the Moon is a potentially vital resource for future lunar bases and
longer-range space exploration. Effective use of the resource depends on developing an
understanding of where and how within the regolith the water is formed and retained. Solar
wind hydrogen, which can form molecular hydrogen, water and/or hydroxyl on the lunar
surface, reacts and is retained differently depending on regolith mineral content, thermal
history, and other variables. Here we present transmission electron microscopy analyses of
Apollo lunar soil 79221 that reveal solar-wind hydrogen concentrated in vesicles as molecular
hydrogen in the calcium-phosphates apatite and merrillite. The location of the vesicles in the
space weathered grain rims offers a clear link between the vesicle contents and solar wind
irradiation, as well as individual grain thermal histories. Hydrogen stored in grain rims is a
source for volatiles released in the exosphere during impacts.
The divergent fates of primitive hydrospheric water on Earth and MarsSérgio Sacani
Despite active transport into Earth’s mantle, water has been
present on our planet’s surface for most of geological time1,2
.
Yet water disappeared from the Martian surface soon after its
formation. Although some of the water on Mars was lost to space
via photolysis following the collapse of the planet’s magnetic field3–5,
the widespread serpentinization of Martian crust6,7
suggests that
metamorphic hydration reactions played a critical part in the
sequestration of the crust. Here we quantify the relative volumes
of water that could be removed from each planet’s surface via the
burial and metamorphism of hydrated mafic crusts, and calculate
mineral transition-induced bulk-density changes at conditions
of elevated pressure and temperature for each. The metamorphic
mineral assemblages in relatively FeO-rich Martian lavas can
hold about 25 per cent more structurally bound water than those
in metamorphosed terrestrial basalts, and can retain it at greater
depths within Mars. Our calculations suggest that in excess of
9 per cent by volume of the Martian mantle may contain hydrous
mineral species as a consequence of surface reactions, compared to
about 4 per cent by volume of Earth’s mantle. Furthermore, neither
primitive nor evolved hydrated Martian crust show noticeably
different bulk densities compared to their anhydrous equivalents,
in contrast to hydrous mafic terrestrial crust, which transforms
to denser eclogite upon dehydration. This would have allowed
efficient overplating and burial of early Martian crust in a stagnantlid
tectonic regime, in which the lithosphere comprised a single
tectonic plate, with only the warmer, lower crust involved in mantle
convection. This provided an important sink for hydrospheric water
and a mechanism for oxidizing the Martian mantle. Conversely,
relatively buoyant mafic crust and hotter geothermal gradients on
Earth reduced the potential for upper-mantle hydration early in
its geological history, leading to water being retained close to its
surface, and thus creating conditions conducive for the evolution
of complex multicellular life
The synthesis and characterization of three new metal chalcogenide aerogels, Chalcogels,
AFe3Zn3S17 (A= Na, K, or Rb) is described. Alkali metal polychalcogenides (Na2S5, K2S5, or Rb2S5)
reactwith metal acetate like Fe(OAc)2 and Zn(OAc)2in formamide solutionforming extended polymeric
frameworks by gelation. Chalcogels obtained aftersupercritical drying have BET surface areas of
430, 444, and 435 m
2
/g for NaFe3Zn3S17, KFe3Zn3S17, and RbFe3Zn3S17, respectively. The effect of the
counter ions (K, Na, and Rb) wasstudied by examined the adsorption capacities of the resulting
chalcogels toward different gases and volatile organic compounds. The measurements showed that
CO2 and toluene adsorption capacities increase with the polarizability of the surface atoms in the
following order: Rb chalcogel> K chalcogel> Na chalcogel.This finding reveals a trend based on
cation size and acid–base surface properties that might have a significant impact on altering
adsorptive properties of chalcogels by using more polarizable counter ions.
ZEISES SALT - KPtCl3(C 2 H 4) Paper #3November 18,.docxdanielfoster65629
ZEISE'S SALT - KPtCl3(C 2 H 4) Paper #3
November 18, 2014
ZEISE'S SALT - KPtCl3(C 2 H 4) Paper #3
November 18, 2014
ZEISE'S SALT - KPtCl3(C 2 H 4)
This is the first metal complex identified as an organometallic compound KPtCl3(C 2 H 4) obtained from reaction of ethylene with platinum (II) chloride by William Zeise in 1825. It was not until much later (1951–1952) that the correct structure of Zeise's compound was reported in connection with the structure of a metallocene compound known as ferrocene. The anion of this air-stable, yellow, coordination complex contains an η2-ethylene ligand and features a platinum atom with a square planar geometry. Zeise's salt is of historical importance in the area of organometallic chemistry as one of the first examples of an alkene complex and that is the major reason for selecting this title.
INTRODUCTION
Inorganic chemistry is the study of the synthesis and behaviour of inorganic and organometallic compounds. This field covers all chemical compounds except the myriad organic compounds (carbon based compounds, usually containing C-H bonds), which are the subjects of organic chemistry.
Organometallic compounds are considered to contain the M-C-H group. The metal (M) in these species can either be a main group element or a transition metal. Operationally, the definition of an organometallic compound is more relaxed to include also highly lipophilic complexes such as metal carbonyls and even metal alkoxides.
In organometallic compounds, most p-electrons of transition metals conform to an empirical rule called the 18-electron rule. This rule assumes that the metal atom accepts from its ligands the number of electrons needed in order for it to attain the electronic configuration of the next noble gas. It assumes that the valence shells of the metal atom will contain 18 electrons. Thus, the sum of the number of d electrons plus the number of electrons supplied by the ligands will be 18. Ferrocene, for example, has 6 d electrons from Fe(II), plus 2 × 6 electrons from the two 5-membered rings, for a total of 18.
Zeise's salt is a coordination compound, K+ ion and water molecule is present outside the coordination sphere. Both, the Cl-ion and ethylene are coordinated with Platinum ion, hence inside the coordination sphere. Molecular formula of the salt is given as K[PtCl3(C2H4)]·H2O
ZEISE'S SALT PREPARATION
W. C. Zeise, a professor at the University of Copenhagen was the first person to prepare zeise’s salt, he prepared this compound in 1820s while investigating the reaction of PtCl4 with boiling ethanol, and proposed that the resulting compound contained ethylene. in 1868 Birnbaum prepared the complex using ethylene. Zeise’s salt compound is now commercially available as a hydrate. Hydrates are inorganic salts "containing water molecules combined in a definite ratio as an integral part of the crystal that are either bound to a metal center or that have crystallized with the metal .
International Journal of Engineering Research and Development (IJERD)IJERD Editor
journal publishing, how to publish research paper, Call For research paper, international journal, publishing a paper, IJERD, journal of science and technology, how to get a research paper published, publishing a paper, publishing of journal, publishing of research paper, reserach and review articles, IJERD Journal, How to publish your research paper, publish research paper, open access engineering journal, Engineering journal, Mathemetics journal, Physics journal, Chemistry journal, Computer Engineering, Computer Science journal, how to submit your paper, peer reviw journal, indexed journal, reserach and review articles, engineering journal, www.ijerd.com, research journals,
yahoo journals, bing journals, International Journal of Engineering Research and Development, google journals, hard copy of journal
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
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.
More Related Content
Similar to Earth’s volatile contents established by melting and vaporization
The divergent fates of primitive hydrospheric water on Earth and MarsSérgio Sacani
Despite active transport into Earth’s mantle, water has been
present on our planet’s surface for most of geological time1,2
.
Yet water disappeared from the Martian surface soon after its
formation. Although some of the water on Mars was lost to space
via photolysis following the collapse of the planet’s magnetic field3–5,
the widespread serpentinization of Martian crust6,7
suggests that
metamorphic hydration reactions played a critical part in the
sequestration of the crust. Here we quantify the relative volumes
of water that could be removed from each planet’s surface via the
burial and metamorphism of hydrated mafic crusts, and calculate
mineral transition-induced bulk-density changes at conditions
of elevated pressure and temperature for each. The metamorphic
mineral assemblages in relatively FeO-rich Martian lavas can
hold about 25 per cent more structurally bound water than those
in metamorphosed terrestrial basalts, and can retain it at greater
depths within Mars. Our calculations suggest that in excess of
9 per cent by volume of the Martian mantle may contain hydrous
mineral species as a consequence of surface reactions, compared to
about 4 per cent by volume of Earth’s mantle. Furthermore, neither
primitive nor evolved hydrated Martian crust show noticeably
different bulk densities compared to their anhydrous equivalents,
in contrast to hydrous mafic terrestrial crust, which transforms
to denser eclogite upon dehydration. This would have allowed
efficient overplating and burial of early Martian crust in a stagnantlid
tectonic regime, in which the lithosphere comprised a single
tectonic plate, with only the warmer, lower crust involved in mantle
convection. This provided an important sink for hydrospheric water
and a mechanism for oxidizing the Martian mantle. Conversely,
relatively buoyant mafic crust and hotter geothermal gradients on
Earth reduced the potential for upper-mantle hydration early in
its geological history, leading to water being retained close to its
surface, and thus creating conditions conducive for the evolution
of complex multicellular life
The synthesis and characterization of three new metal chalcogenide aerogels, Chalcogels,
AFe3Zn3S17 (A= Na, K, or Rb) is described. Alkali metal polychalcogenides (Na2S5, K2S5, or Rb2S5)
reactwith metal acetate like Fe(OAc)2 and Zn(OAc)2in formamide solutionforming extended polymeric
frameworks by gelation. Chalcogels obtained aftersupercritical drying have BET surface areas of
430, 444, and 435 m
2
/g for NaFe3Zn3S17, KFe3Zn3S17, and RbFe3Zn3S17, respectively. The effect of the
counter ions (K, Na, and Rb) wasstudied by examined the adsorption capacities of the resulting
chalcogels toward different gases and volatile organic compounds. The measurements showed that
CO2 and toluene adsorption capacities increase with the polarizability of the surface atoms in the
following order: Rb chalcogel> K chalcogel> Na chalcogel.This finding reveals a trend based on
cation size and acid–base surface properties that might have a significant impact on altering
adsorptive properties of chalcogels by using more polarizable counter ions.
ZEISES SALT - KPtCl3(C 2 H 4) Paper #3November 18,.docxdanielfoster65629
ZEISE'S SALT - KPtCl3(C 2 H 4) Paper #3
November 18, 2014
ZEISE'S SALT - KPtCl3(C 2 H 4) Paper #3
November 18, 2014
ZEISE'S SALT - KPtCl3(C 2 H 4)
This is the first metal complex identified as an organometallic compound KPtCl3(C 2 H 4) obtained from reaction of ethylene with platinum (II) chloride by William Zeise in 1825. It was not until much later (1951–1952) that the correct structure of Zeise's compound was reported in connection with the structure of a metallocene compound known as ferrocene. The anion of this air-stable, yellow, coordination complex contains an η2-ethylene ligand and features a platinum atom with a square planar geometry. Zeise's salt is of historical importance in the area of organometallic chemistry as one of the first examples of an alkene complex and that is the major reason for selecting this title.
INTRODUCTION
Inorganic chemistry is the study of the synthesis and behaviour of inorganic and organometallic compounds. This field covers all chemical compounds except the myriad organic compounds (carbon based compounds, usually containing C-H bonds), which are the subjects of organic chemistry.
Organometallic compounds are considered to contain the M-C-H group. The metal (M) in these species can either be a main group element or a transition metal. Operationally, the definition of an organometallic compound is more relaxed to include also highly lipophilic complexes such as metal carbonyls and even metal alkoxides.
In organometallic compounds, most p-electrons of transition metals conform to an empirical rule called the 18-electron rule. This rule assumes that the metal atom accepts from its ligands the number of electrons needed in order for it to attain the electronic configuration of the next noble gas. It assumes that the valence shells of the metal atom will contain 18 electrons. Thus, the sum of the number of d electrons plus the number of electrons supplied by the ligands will be 18. Ferrocene, for example, has 6 d electrons from Fe(II), plus 2 × 6 electrons from the two 5-membered rings, for a total of 18.
Zeise's salt is a coordination compound, K+ ion and water molecule is present outside the coordination sphere. Both, the Cl-ion and ethylene are coordinated with Platinum ion, hence inside the coordination sphere. Molecular formula of the salt is given as K[PtCl3(C2H4)]·H2O
ZEISE'S SALT PREPARATION
W. C. Zeise, a professor at the University of Copenhagen was the first person to prepare zeise’s salt, he prepared this compound in 1820s while investigating the reaction of PtCl4 with boiling ethanol, and proposed that the resulting compound contained ethylene. in 1868 Birnbaum prepared the complex using ethylene. Zeise’s salt compound is now commercially available as a hydrate. Hydrates are inorganic salts "containing water molecules combined in a definite ratio as an integral part of the crystal that are either bound to a metal center or that have crystallized with the metal .
International Journal of Engineering Research and Development (IJERD)IJERD Editor
journal publishing, how to publish research paper, Call For research paper, international journal, publishing a paper, IJERD, journal of science and technology, how to get a research paper published, publishing a paper, publishing of journal, publishing of research paper, reserach and review articles, IJERD Journal, How to publish your research paper, publish research paper, open access engineering journal, Engineering journal, Mathemetics journal, Physics journal, Chemistry journal, Computer Engineering, Computer Science journal, how to submit your paper, peer reviw journal, indexed journal, reserach and review articles, engineering journal, www.ijerd.com, research journals,
yahoo journals, bing journals, International Journal of Engineering Research and Development, google journals, hard copy of journal
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
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.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243Sérgio Sacani
The recently reported observation of VFTS 243 is the first example of a massive black-hole binary
system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙)
and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete
collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to
constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence
level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution
that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal
kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small
neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Detectability of Solar Panels as a TechnosignatureSérgio Sacani
In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like
exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the
UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept
like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide
the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand
assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope.
Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the
ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed
to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel
coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev
Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even
with much larger populations than today, the total energy use of human civilization would be orders of
magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev
Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population
levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization
as imagined in the Fermi paradox may not exist.
Jet reorientation in central galaxies of clusters and groups: insights from V...Sérgio Sacani
Recent observations of galaxy clusters and groups with misalignments between their central AGN jets
and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet – bubble
connection in cooling cores, and the processes responsible for jet realignment. To investigate the
frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and
groups. Using VLBA radio data we measure the parsec-scale position angle of the jets, and compare
it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample
and selected subsets, we consistently find that there is a 30% – 38% chance to find a misalignment
larger than ∆Ψ = 45◦ when observing a cluster/group with a detected jet and at least one cavity. We
determine that projection may account for an apparently large ∆Ψ only in a fraction of objects (∼35%),
and given that gas dynamical disturbances (as sloshing) are found in both aligned and misaligned
systems, we exclude environmental perturbation as the main driver of cavity – jet misalignment.
Moreover, we find that large misalignments (up to ∼ 90◦
) are favored over smaller ones (45◦ ≤ ∆Ψ ≤
70◦
), and that the change in jet direction can occur on timescales between one and a few tens of Myr.
We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we
discuss several engine-based mechanisms that may cause these dramatic changes.
The solar dynamo begins near the surfaceSérgio Sacani
The magnetic dynamo cycle of the Sun features a distinct pattern: a propagating
region of sunspot emergence appears around 30° latitude and vanishes near the
equator every 11 years (ref. 1). Moreover, longitudinal flows called torsional oscillations
closely shadow sunspot migration, undoubtedly sharing a common cause2. Contrary
to theories suggesting deep origins of these phenomena, helioseismology pinpoints
low-latitude torsional oscillations to the outer 5–10% of the Sun, the near-surface
shear layer3,4. Within this zone, inwardly increasing differential rotation coupled with
a poloidal magnetic field strongly implicates the magneto-rotational instability5,6,
prominent in accretion-disk theory and observed in laboratory experiments7.
Together, these two facts prompt the general question: whether the solar dynamo is
possibly a near-surface instability. Here we report strong affirmative evidence in stark
contrast to traditional models8 focusing on the deeper tachocline. Simple analytic
estimates show that the near-surface magneto-rotational instability better explains
the spatiotemporal scales of the torsional oscillations and inferred subsurface
magnetic field amplitudes9. State-of-the-art numerical simulations corroborate these
estimates and reproduce hemispherical magnetic current helicity laws10. The dynamo
resulting from a well-understood near-surface phenomenon improves prospects
for accurate predictions of full magnetic cycles and space weather, affecting the
electromagnetic infrastructure of Earth.
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Mat...Sérgio Sacani
In the Nice model of solar system formation, Uranus and Neptune undergo an orbital upheaval,
sweeping through a planetesimal disk. The region of the disk from which material is accreted by
the ice giants during this phase of their evolution has not previously been identified. We perform
direct N-body orbital simulations of the four giant planets to determine the amount and origin of solid
accretion during this orbital upheaval. We find that the ice giants undergo an extreme bombardment
event, with collision rates as much as ∼3 per hour assuming km-sized planetesimals, increasing the
total planet mass by up to ∼0.35%. In all cases, the initially outermost ice giant experiences the
largest total enhancement. We determine that for some plausible planetesimal properties, the resulting
atmospheric enrichment could potentially produce sufficient latent heat to alter the planetary cooling
timescale according to existing models. Our findings suggest that substantial accretion during this
phase of planetary evolution may have been sufficient to impact the atmospheric composition and
thermal evolution of the ice giants, motivating future work on the fate of deposited solid material.
Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...Sérgio Sacani
The highest priority recommendation of the Astro2020 Decadal Survey for space-based astronomy
was the construction of an observatory capable of characterizing habitable worlds. In this paper series
we explore the detectability of and interference from exomoons and exorings serendipitously observed
with the proposed Habitable Worlds Observatory (HWO) as it seeks to characterize exoplanets, starting
in this manuscript with Earth-Moon analog mutual events. Unlike transits, which only occur in systems
viewed near edge-on, shadow (i.e., solar eclipse) and lunar eclipse mutual events occur in almost every
star-planet-moon system. The cadence of these events can vary widely from ∼yearly to multiple events
per day, as was the case in our younger Earth-Moon system. Leveraging previous space-based (EPOXI)
lightcurves of a Moon transit and performance predictions from the LUVOIR-B concept, we derive
the detectability of Moon analogs with HWO. We determine that Earth-Moon analogs are detectable
with observation of ∼2-20 mutual events for systems within 10 pc, and larger moons should remain
detectable out to 20 pc. We explore the extent to which exomoon mutual events can mimic planet
features and weather. We find that HWO wavelength coverage in the near-IR, specifically in the 1.4 µm
water band where large moons can outshine their host planet, will aid in differentiating exomoon signals
from exoplanet variability. Finally, we predict that exomoons formed through collision processes akin
to our Moon are more likely to be detected in younger systems, where shorter orbital periods and
favorable geometry enhance the probability and frequency of mutual events.
Emergent ribozyme behaviors in oxychlorine brines indicate a unique niche for...Sérgio Sacani
Mars is a particularly attractive candidate among known astronomical objects
to potentially host life. Results from space exploration missions have provided
insights into Martian geochemistry that indicate oxychlorine species, particularly perchlorate, are ubiquitous features of the Martian geochemical landscape. Perchlorate presents potential obstacles for known forms of life due to
its toxicity. However, it can also provide potential benefits, such as producing
brines by deliquescence, like those thought to exist on present-day Mars. Here
we show perchlorate brines support folding and catalysis of functional RNAs,
while inactivating representative protein enzymes. Additionally, we show
perchlorate and other oxychlorine species enable ribozyme functions,
including homeostasis-like regulatory behavior and ribozyme-catalyzed
chlorination of organic molecules. We suggest nucleic acids are uniquely wellsuited to hypersaline Martian environments. Furthermore, Martian near- or
subsurface oxychlorine brines, and brines found in potential lifeforms, could
provide a unique niche for biomolecular evolution.
Continuum emission from within the plunging region of black hole discsSérgio Sacani
The thermal continuum emission observed from accreting black holes across X-ray bands has the potential to be leveraged as a
powerful probe of the mass and spin of the central black hole. The vast majority of existing ‘continuum fitting’ models neglect
emission sourced at and within the innermost stable circular orbit (ISCO) of the black hole. Numerical simulations, however,
find non-zero emission sourced from these regions. In this work, we extend existing techniques by including the emission
sourced from within the plunging region, utilizing new analytical models that reproduce the properties of numerical accretion
simulations. We show that in general the neglected intra-ISCO emission produces a hot-and-small quasi-blackbody component,
but can also produce a weak power-law tail for more extreme parameter regions. A similar hot-and-small blackbody component
has been added in by hand in an ad hoc manner to previous analyses of X-ray binary spectra. We show that the X-ray spectrum
of MAXI J1820+070 in a soft-state outburst is extremely well described by a full Kerr black hole disc, while conventional
models that neglect intra-ISCO emission are unable to reproduce the data. We believe this represents the first robust detection of
intra-ISCO emission in the literature, and allows additional constraints to be placed on the MAXI J1820 + 070 black hole spin
which must be low a• < 0.5 to allow a detectable intra-ISCO region. Emission from within the ISCO is the dominant emission
component in the MAXI J1820 + 070 spectrum between 6 and 10 keV, highlighting the necessity of including this region. Our
continuum fitting model is made publicly available.
WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 RpSérgio Sacani
Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical
mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed
as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple
groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this
planet’s outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the
target set, demonstrating the outflow extends at least 5.8 × 105 km or 7.5 Rp This detection is significantly longer
than previous observations, which report an outflow extending ∼2.2 planet radii just 1 yr prior. The outflow is
blueshifted by −23 km s−1 in the planetary rest frame. We estimate a current mass-loss rate of 1 M⊕ Gyr−1
. Our
observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind.
However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or
differences in instrumental precision.
X-rays from a Central “Exhaust Vent” of the Galactic Center ChimneySérgio Sacani
Using deep archival observations from the Chandra X-ray Observatory, we present an analysis of
linear X-ray-emitting features located within the southern portion of the Galactic center chimney,
and oriented orthogonal to the Galactic plane, centered at coordinates l = 0.08◦
, b = −1.42◦
. The
surface brightness and hardness ratio patterns are suggestive of a cylindrical morphology which may
have been produced by a plasma outflow channel extending from the Galactic center. Our fits of the
feature’s spectra favor a complex two-component model consisting of thermal and recombining plasma
components, possibly a sign of shock compression or heating of the interstellar medium by outflowing
material. Assuming a recombining plasma scenario, we further estimate the cooling timescale of this
plasma to be on the order of a few hundred to thousands of years, leading us to speculate that a
sequence of accretion events onto the Galactic Black Hole may be a plausible quasi-continuous energy
source to sustain the observed morphology
Nutraceutical market, scope and growth: Herbal drug technologyLokesh Patil
As consumer awareness of health and wellness rises, the nutraceutical market—which includes goods like functional meals, drinks, and dietary supplements that provide health advantages beyond basic nutrition—is growing significantly. As healthcare expenses rise, the population ages, and people want natural and preventative health solutions more and more, this industry is increasing quickly. Further driving market expansion are product formulation innovations and the use of cutting-edge technology for customized nutrition. With its worldwide reach, the nutraceutical industry is expected to keep growing and provide significant chances for research and investment in a number of categories, including vitamins, minerals, probiotics, and herbal supplements.
DERIVATION OF MODIFIED BERNOULLI EQUATION WITH VISCOUS EFFECTS AND TERMINAL V...Wasswaderrick3
In this book, we use conservation of energy techniques on a fluid element to derive the Modified Bernoulli equation of flow with viscous or friction effects. We derive the general equation of flow/ velocity and then from this we derive the Pouiselle flow equation, the transition flow equation and the turbulent flow equation. In the situations where there are no viscous effects , the equation reduces to the Bernoulli equation. From experimental results, we are able to include other terms in the Bernoulli equation. We also look at cases where pressure gradients exist. We use the Modified Bernoulli equation to derive equations of flow rate for pipes of different cross sectional areas connected together. We also extend our techniques of energy conservation to a sphere falling in a viscous medium under the effect of gravity. We demonstrate Stokes equation of terminal velocity and turbulent flow equation. We look at a way of calculating the time taken for a body to fall in a viscous medium. We also look at the general equation of terminal velocity.
Comparing Evolved Extractive Text Summary Scores of Bidirectional Encoder Rep...University of Maribor
Slides from:
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Track: Artificial Intelligence
https://www.etran.rs/2024/en/home-english/
(May 29th, 2024) Advancements in Intravital Microscopy- Insights for Preclini...Scintica Instrumentation
Intravital microscopy (IVM) is a powerful tool utilized to study cellular behavior over time and space in vivo. Much of our understanding of cell biology has been accomplished using various in vitro and ex vivo methods; however, these studies do not necessarily reflect the natural dynamics of biological processes. Unlike traditional cell culture or fixed tissue imaging, IVM allows for the ultra-fast high-resolution imaging of cellular processes over time and space and were studied in its natural environment. Real-time visualization of biological processes in the context of an intact organism helps maintain physiological relevance and provide insights into the progression of disease, response to treatments or developmental processes.
In this webinar we give an overview of advanced applications of the IVM system in preclinical research. IVIM technology is a provider of all-in-one intravital microscopy systems and solutions optimized for in vivo imaging of live animal models at sub-micron resolution. The system’s unique features and user-friendly software enables researchers to probe fast dynamic biological processes such as immune cell tracking, cell-cell interaction as well as vascularization and tumor metastasis with exceptional detail. This webinar will also give an overview of IVM being utilized in drug development, offering a view into the intricate interaction between drugs/nanoparticles and tissues in vivo and allows for the evaluation of therapeutic intervention in a variety of tissues and organs. This interdisciplinary collaboration continues to drive the advancements of novel therapeutic strategies.
This presentation explores a brief idea about the structural and functional attributes of nucleotides, the structure and function of genetic materials along with the impact of UV rays and pH upon them.
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...Ana Luísa Pinho
Functional Magnetic Resonance Imaging (fMRI) provides means to characterize brain activations in response to behavior. However, cognitive neuroscience has been limited to group-level effects referring to the performance of specific tasks. To obtain the functional profile of elementary cognitive mechanisms, the combination of brain responses to many tasks is required. Yet, to date, both structural atlases and parcellation-based activations do not fully account for cognitive function and still present several limitations. Further, they do not adapt overall to individual characteristics. In this talk, I will give an account of deep-behavioral phenotyping strategies, namely data-driven methods in large task-fMRI datasets, to optimize functional brain-data collection and improve inference of effects-of-interest related to mental processes. Key to this approach is the employment of fast multi-functional paradigms rich on features that can be well parametrized and, consequently, facilitate the creation of psycho-physiological constructs to be modelled with imaging data. Particular emphasis will be given to music stimuli when studying high-order cognitive mechanisms, due to their ecological nature and quality to enable complex behavior compounded by discrete entities. I will also discuss how deep-behavioral phenotyping and individualized models applied to neuroimaging data can better account for the subject-specific organization of domain-general cognitive systems in the human brain. Finally, the accumulation of functional brain signatures brings the possibility to clarify relationships among tasks and create a univocal link between brain systems and mental functions through: (1) the development of ontologies proposing an organization of cognitive processes; and (2) brain-network taxonomies describing functional specialization. To this end, tools to improve commensurability in cognitive science are necessary, such as public repositories, ontology-based platforms and automated meta-analysis tools. I will thus discuss some brain-atlasing resources currently under development, and their applicability in cognitive as well as clinical neuroscience.
Toxic effects of heavy metals : Lead and Arsenicsanjana502982
Heavy metals are naturally occuring metallic chemical elements that have relatively high density, and are toxic at even low concentrations. All toxic metals are termed as heavy metals irrespective of their atomic mass and density, eg. arsenic, lead, mercury, cadmium, thallium, chromium, etc.