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The document outlines a plan to colonize Mars by sending unmanned and manned missions. It discusses why colonizing Mars is desirable, such as preparing for Earth becoming uninhabitable. The plan is to send ships with fuel, living quarters, and vehicles to return to Earth. Additional missions would build a permanent habitat. Mars' atmosphere and climate would need to be altered through greenhouse gases and microbes to become habitable. While colonization will be challenging and costly, the document argues it is possible within the next 100 years based on current research progress.
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Discovery of An Apparent Red, High-Velocity Type Ia Supernova at 𝐳 = 2.9 wi...
We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
Compositions of iron-meteorite parent bodies constrainthe structure of the pr...
Magmatic iron-meteorite parent bodies are the earliest planetesimals in the Solar System,and they preserve information about conditions and planet-forming processes in thesolar nebula. In this study, we include comprehensive elemental compositions andfractional-crystallization modeling for iron meteorites from the cores of five differenti-ated asteroids from the inner Solar System. Together with previous results of metalliccores from the outer Solar System, we conclude that asteroidal cores from the outerSolar System have smaller sizes, elevated siderophile-element abundances, and simplercrystallization processes than those from the inner Solar System. These differences arerelated to the formation locations of the parent asteroids because the solar protoplane-tary disk varied in redox conditions, elemental distributions, and dynamics at differentheliocentric distances. Using highly siderophile-element data from iron meteorites, wereconstruct the distribution of calcium-aluminum-rich inclusions (CAIs) across theprotoplanetary disk within the first million years of Solar-System history. CAIs, the firstsolids to condense in the Solar System, formed close to the Sun. They were, however,concentrated within the outer disk and depleted within the inner disk. Future modelsof the structure and evolution of the protoplanetary disk should account for this dis-tribution pattern of CAIs.
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Presentation given at the official farewell of Prof Ken Gillet at Wageningen on 13 June 2024
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDS
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
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- 1. The Mission to Colonize Mars A home away from home… (Yes, I know there aren’t oceans on Mars, but come on…the background looks cool)
- 2. Outline • Introduction – Background information • Why do we want to try this? • How do we plan on getting there? • How do we make it inhabitable? • Is it possible? Will it happen? • Conclusion
- 3. Introduction • Originally observed as a red star – represented evil and war • Became the focus of science fiction – Stimulated public interest • Mariner 3 sent to Mars – 1964 • Viking landers map surface – 1975 – No evidence of life • Mars pathfinder – 1997 • Meteorite from Mars – signs of life Images of the Pathfinder landing site
- 4. Why do we want to try? • Earth may someday become uninhabitable – Overpopulation, resources, environment • Information about the universe and life – Implications on our place in the universe • Larger frontier and different environment • Developments that may change the way we live • Symbolism of the advancement and cooperation of mankind • Job opportunities and global economy
- 5. How do we plan to get there? • Need: way to get there, place to stay, way to get back – Fuel, food, air • 1st year: Send 1 or 2 unmanned ships – MAV(Mars Ascent Vehicle), ERV(Earth Return Vehicle), and an unmanned habitat • 3rd year: Send 1 or 2 unmanned, 1 manned – Same first ships, last contains four astronauts • 5th year and every odd year after: repeat – Continuous habitation on Mars • MAV produces it’s own fuel from the atmosphere (Carbon Dioxide and Hydrogen -> Methane) • Other options: Brute force (one huge ship with everything), one-way trip (astronauts never return) Diagram of the possible missions to mars discussed (Orbital Rendezvous with in-situ (on site) propellants ).
- 6. How can Mars become habitable? • Problems: – Only known water sources in ice caps and permafrost beneath the surface – Cannot breathe in current atmosphere – Weather is much too harsh (average of -60 degree Celsius temperature, for example) • Solutions: – Release manufactured greenhouse gases • Temperature raises to 0 degrees Celsius and higher • Frozen carbon dioxide sublimes to gas, increasing pressure and raising temperature • Water melts, causing a hydrological cycle – Microbes released to form a biosphere and produce oxygen • Moss and plant life begins Timeline diagram from left to right of the terraformation of Mars
- 7. Is it possible, and will it happen? • Based on current ideas and research, it is highly possible. • Opposition in the form of cost, purpose, and risk. – Originally estimated at $450 billion, now estimated between $20 - $50 billion for three missions. – Can make it significantly less risky by use of in-situ propellant and orbital rendezvous. • Plan on making manned-missions – http://mars.jpl.nasa.gov/mer/mission/timeline.html for timelines and information • Some say it will take no more than 100 years to terraform, some say almost 1 million. Either way, it will probably be several decades from now, at least, before we might begin.
- 8. Conclusion • Colonization of Mars is certainly possible, and definitely a consideration for the future. • There are many reasons for colonizing Mars, some very practical. • Though colonization will not likely be seen in our lifetime, the future could hold a new Earth-like planet, colonized the surface-over by humans.
- 9. References • http://www.ibiblio.org/astrobiology/index.php?p age=mars03’ • http://www.ucls.uchicago.edu/MartianSunTimes/ • http://www.ibiblio.org/astrobiology/index.php?p age=mars04 • http://mars.jpl.nasa.gov/MPF/index0.html • http://www- geology.ucdavis.edu/~GEL36/GEL36Honors01/co st/cost.html