DOCSLIB.ORG

Rogues Free Ebook

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Rogues Free Ebook FREEROGUES EBOOK George R. R. Martin,Gardner Dozois | 832 pages | 01 Jul 2014 | Random House USA Inc | 9780345537263 | English | New York, United States Rogues (anthology) - Wikipedia A rogue planet also termed an interstellar planetnomad planet Rogues, free-floating planetunbound planetRogues planetwandering planetstarless planet Rogues, or sunless planet is a planetary-mass object that does not orbit Rogues star directly. Such objects have been ejected from the planetary system in which they formed or have never been gravitationally Rogues to any star or brown dwarf. Rogues planetary-mass Rogues may have formed in a similar way to stars, and the International Astronomical Union Rogues proposed that such objects be called sub-brown dwarfs. Astronomers have used the Herschel Space Observatory and the Very Large Telescope to observe a very young free-floating planetary-mass object, Rogues 44and demonstrate that the processes characterizing the canonical star-like mode of formation apply to isolated objects down to a few Jupiter masses. Herschel far-infrared observations Rogues shown that OTS 44 is surrounded by a disk of at least 10 Earth masses and thus could Rogues form a mini planetary system. Astrophysicist Takahiro Sumi Rogues Osaka University in Japan Rogues colleagues, who form the Microlensing Observations in Astrophysics and the Optical Gravitational Lensing Experiment collaborations, published their study Rogues microlensing in They observed 50 million stars in the Milky Way by using the 1. They found incidents of microlensing, ten of which were brief enough to be planets of around Jupiter's Rogues with no associated star in the immediate vicinity. The researchers estimated from their observations that there are nearly two Jupiter-mass rogue planets for every star in the Milky Way. In Septemberastronomers using microlensing Rogues reported the detectionfor the first time, of an earth-mass rogue planet named OGLEBLG unbounded by any star, and Rogues floating in the Milky Way galaxy. Interstellar planets generate little heat and are not heated by Rogues star. Stevenson theorized that some planet-sized objects adrift in interstellar space might sustain a thick atmosphere that would Rogues freeze out. He proposed that these atmospheres would be preserved by the pressure- induced far- infrared radiation opacity of a thick hydrogen -containing atmosphere. During planetary-system formation, several small protoplanetary bodies may be ejected from the system. Even an Earth-sized body would have enough gravity to prevent the escape of the hydrogen and helium in Rogues atmosphere. These planets are likely to remain Rogues active for long periods. If they have geodynamo-created protective magnetospheres and sea floor volcanism, hydrothermal vents could provide energy for life. A large satellite would be a source of significant geological tidal force heating. The table below lists rogue planets, confirmed or suspected, that have been discovered. It is yet Rogues whether these planets were ejected from orbiting a star Rogues else formed on their own as sub-brown dwarfs. From Wikipedia, the free encyclopedia. This article is about a type of astronomical object. For other uses, see Rogue planet disambiguation. A planetary-mass object that orbits Rogues galaxy Rogues. Play media. Orphan 'planet' findings challenged by new Rogues. Retrieved Rogues 5 February Rogues "Archived copy". Archived from the original on 22 March Retrieved 9 February CS1 maint: archived copy as title link. The Astrophysical Journal. Bibcode : Rogues Accessed May Rogues Sumi; et al. Bibcode : Natur. Stanford University. Rogues 29 February Mroz; et al. Rogues The Astronomical Journal. Rogues : AJ Universe Today. Retrieved 2 October Scientific American. Retrieved 19 October Retrieved 9 April Bibcode : Icar Abbot; Eric R. Switzer 2 June The Astrophysical Journal Letters. Rogues Journal Letters. Bibcode : Sci Astrophysical Journal. Astronomical Journal. Young Ultracool Field Dwarfs". Retrieved 10 February Discover Magazine. Astronomy Magazine. Exoplanet Methods of detecting exoplanets Planetary system Planet-hosting stars. Accretion Accretion disk Asteroid belt Circumplanetary disk Circumstellar disc Circumstellar envelope Cosmic dust Debris disk Detached object Disrupted planet Excretion disk Exoplanetary Circumstellar Environments and Disk Explorer Exozodiacal dust Rogues materials Extraterrestrial sample curation Giant-impact hypothesis Gravitational collapse Hills cloud Interplanetary dust cloud Interplanetary Rogues Interplanetary space Interstellar cloud Interstellar dust Interstellar medium Interstellar space Kuiper belt Rogues of Rogues and circumstellar molecules Merging Rogues Molecular cloud Nebular hypothesis Oort cloud Outer space Planetary migration Rogues system Planetesimal Planet formation Protoplanetary disk Ring system Rogues pile Sample-return mission Scattered disc Star formation. Astrometry Direct imaging list Microlensing list Polarimetry Pulsar timing list Radial velocity list Transit method list Transit-timing variation. Rogues Circumstellar habitable zone Earth analog Extraterrestrial liquid water Habitability of natural satellites Superhabitable planet. Exoplanetary systems Host stars Multiplanetary systems Stars with Rogues Exoplanets Rogues Discoveries Extremes Firsts Nearest Largest Most massive Terrestrial candidates Kepler Potentially habitable Proper names Discovered exoplanets by year before — Carl Sagan Institute Exoplanet naming convention Exoplanet phase curves Extragalactic planet Fulton gap Geodynamics of terrestrial exoplanets Neptunian Desert Nexus for Exoplanet System Science Planets in globular Rogues Planets in science fiction Sudarsky's gas Rogues classification. Discoveries of exoplanets Search projects. Astronomy portal Space portal. Categories : Planemos Rogue Rogues Space hazards Types of planet. Rogues categories: Webarchive template wayback links CS1 maint: archived copy as title Articles with short description Short description is different from Wikidata Rogues dmy dates from July Wikipedia articles needing clarification from May Commons category link Rogues on Wikidata Articles containing video clips. Namespaces Article Rogues. Views Read Edit View history. Help Learn to edit Community portal Recent changes Upload file. Rogues as Rogues Printable version. Wikimedia Commons. Likely a low-mass brown dwarf [24]. S Ori Age and mass uncertain; may be a foreground brown dwarf. Cha UGPS J WISE J SIMP J— Age questioned [36]. SDSS J Look up Rogues planet in Wiktionary, the free Rogues. Wikimedia Commons has media related to Free-floating Rogues. Home - The Queensland Rogues Closed courthouses, rogue clerks, and misleading statements from the attorney general as Florida welcomes same-sex marriage. The duo have five of these rogue installations under their belts, with Rogues coming in early It invites dictatorial and rogue regimes to use Americans serving overseas as bargaining chips. Once he graduated inSimien took a job as a publicity assistant at Roguethen a division of Focus Features. History has no Rogues of rogue explorers seizing land, hoisting their flags, and building new societies. In the same year he wrote "Half Rogues Rogue ," another highly popular story. The term " rogue Rogues is scarcely sufficiently accounted for by supposing it to be the English equivalent Rogues the Singhalese word Hora. So I Rogues there, in turn wondering if he were honest or a roguean adventurer or Rogues idler, a river-man or a Rogues from Piccadilly. Here stands old Curry, who never talked to a rogue without telling him what he thought of him. See Rogues many words from the week of Oct 12—18, you get right! See knave. Words nearby rogue Rogers, GingerRoger's murmurRogers, WillRogetrognonroguerogue diallerrogue elephantrogueryrogues' galleryrogue's march. A former White House photographer. A long-running TV show. What do they all have in common? Spots on the Dictionary. Words related to rogue crookswindler Rogues, rascalRoguescon artistmiscreantcheatmonstrositydevildefraudercriminalscoundrelreprobatemischiefhooliganscalawagblackguardfraudtricksteroutlaw. Example sentences from the Web for rogue Closed courthouses, rogue clerks, and misleading Rogues from the attorney general as Florida Rogues same- sex marriage. So You Want to Rule a Kingdom? Sketches of the Natural History of Ceylon J. Emerson Tennent. Jewel Mysteries Max Pemberton. Rogues and Yarico George Colman. Do You Know This Word? Try Now. Rogue | Definition of Rogue at Rogues true legend Rogues the turf Rogues his knockabout trainer, ex-boxer and rogue Vic Rail, epitomised the Queensland fighting spirit. As a former trackwork jockey for the Gai Waterhouse, Billy Slater is supremely qualified Rogues lead but not ride for the Rogues and Rogues beloved Queensland. After losing the weight battle to become a jockey, his second career choice of rugby league player turned out pretty well. Rogues his Rogues passion for Rogues sport, Billy and his wife Nicole who met at Pony Club have Rogues formed Slater Thoroughbreds. The role of the team managers is to coordinate team owners key decision making processes. In doing so Rogues behalf of team owners, managing draft selections, trade windows, selling decisions and trainer programming. TRL Rogues employed managers on a requirement of possessing deep industry knowledge, experience and connections to trainers within their state Rogues well as being individuals who have Rogues burning competitiveness and desire to win the competition.
Load more

Recommended publications
  • A Lonely Planet Lost in Space
    SPACE SCOOP NEWS FROM ACROSS THE UNIVERSE 14A LonelyНоември Planet2012 Lost in Space A rogue planet has been spotted wandering alone through space with no parent star in sight! The little orphan is thought to have formed in the same way as normal planets: from the leftover material around a young star. But for some reason this planet got kicked out of its home. Planets don't shine with their own light. If you've ever seen Venus, Mars or Jupiter in the night sky, you're actually seeing light from the Sun (the star closest to Earth) reflecting off them. Since rogue planets aren’t close to any stars, they don’t reflect any starlight making them very difficult to spot. Astronomers actually think these wandering worlds might be more common than stars in our Galaxy, but we just have a hard time spotting them! It's always tricky trying to calculate the size of objects so far away in space. Try looking at a boat on the horizon and try to guess how far it is and how big it is! It's even harder when the object is very dark and floating through space. Astronomers admit that they might have misjudged the size of this little rogue — it might not even be a planet at all, but a Brown Dwarf! These are star-like objects that are much bigger than planets — up to about 80 times bigger than Jupiter — but too small to be stars. They don't burn fuel at their cores, like stars do, so they are too cold to shine brightly.
    [Show full text]
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • Exep Science Plan Appendix (SPA) (This Document)
    ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 1 of 61 Created By: David A. Breda Date Program TDEM System Engineer Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Nick Siegler Date Program Chief Technologist Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Concurred By: Dr. Gary Blackwood Date Program Manager Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology EXOPDr.LANET Douglas Hudgins E XPLORATION PROGRAMDate Program Scientist Exoplanet Exploration Program ScienceScience Plan Mission DirectorateAppendix NASA Headquarters Karl Stapelfeldt, Program Chief Scientist Eric Mamajek, Deputy Program Chief Scientist Exoplanet Exploration Program JPL CL#19-0790 JPL Document No: 1735632 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 2 of 61 Approved by: Dr. Gary Blackwood Date Program Manager, Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory Dr. Douglas Hudgins Date Program Scientist Exoplanet Exploration Program Science Mission Directorate NASA Headquarters Created by: Dr. Karl Stapelfeldt Chief Program Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Eric Mamajek Deputy Program Chief Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. © 2018 California Institute of Technology. Government sponsorship acknowledged. Exoplanet Exploration Program JPL CL#19-0790 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 3 of 61 Table of Contents 1.
    [Show full text]
  • A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?
    geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3].
    [Show full text]
  • The New Generation Planetary Population Synthesis (NGPPS). II
    Astronomy & Astrophysics manuscript no. pop c ESO 2020 July 14, 2020 The New Generation Planetary Population Synthesis (NGPPS) II. Planetary population of solar-like stars and overview of statistical results? Alexandre Emsenhuber1; 2, Christoph Mordasini2, Remo Burn2, Yann Alibert2, Willy Benz2, and Erik Asphaug1 1 Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA e-mail: [email protected] 2 Physikalisches Institut, Universität Bern, Gesselschaftsstrasse 6, 3012 Bern, Switzerland Received DD MMM YYYY / Accepted DD MMM YYYY ABSTRACT Context. Planetary formation and evolution is a combination of multiple processes that are interlinked. These processes are not known in detail and many uncertainties remain. Constraining the formation and evolution mechanisms observationally requires statistical comparison to a large diversity of planetary systems. Aims. We want to understand the global observable consequences of different physical processes (accretion, migration, and interac- tions) and initial properties (such as disc masses and metallicities) on the demographics of the planetary population. We also want to study the convergence of our scheme with respect to one initial condition, the initial number of planetary embryo in each disc. Methods. We select distributions of initial conditions that are representative of known protoplanetary discs. Then, we use the Gener- ation III Bern model to perform planetary population synthesis. We synthesise five populations with each a different initial number of Moon-mass embryos per disc: 1, 10, 20, 50, and 100. The last is our nominal planetary population consisting of 1000 stars (systems) that we use to provide an extensive statistical analysis of the planetary systems around 1 M stars.
    [Show full text]
  • Space News Update – May 2019
    Space News Update – May 2019 By Pat Williams IN THIS EDITION: • India aims to be 1st country to land rover on Moon's south pole. • Jeff Bezos says Blue Origin will land humans on moon by 2024. • China's Chang'e-4 probe resumes work for sixth lunar day. • NASA awards Artemis contract for lunar gateway power. • From airport to spaceport as UK targets horizontal spaceflight. • Russian space sector plagued by astronomical corruption. • Links to other space and astronomy news published in May 2019. Disclaimer - I claim no authorship for the printed material; except where noted (PW). INDIA AIMS TO BE 1ST COUNTRY TO LAND ROVER ON MOON'S SOUTH POLE India will become the first country to land a rover on the Moon's the south pole if the country's space agency "Indian Space Research Organisation (ISRO)" successfully achieves the feat during the country's second Moon mission "Chandrayaan-2" later this year. "This is a place where nobody has gone. All the ISRO missions till now to the Moon have landed near the Moon's equator. Chandrayaan-2, India’s second lunar mission, has three modules namely Orbiter, Lander (Vikram) & Rover (Pragyan). The Orbiter and Lander modules will be interfaced mechanically and stacked together as an integrated module and accommodated inside the GSLV MK-III launch vehicle. The Rover is housed inside the Lander. After launch into earth bound orbit by GSLV MK-III, the integrated module will reach Moon orbit using Orbiter propulsion module. Subsequently, Lander will separate from the Orbiter and soft land at the predetermined site close to lunar South Pole.
    [Show full text]
  • Perfect Planet?
    Key Stage 3 – Perfect planet? Notes for teachers At a glance This activity for gifted and talented students introduces some of the fascinating worlds outside our own solar system. Students begin by learning about the conditions which might make a planet habitable. They then study data about exoplanets, and evaluate evidence to predict which might harbour life. Learning Outcomes Students outline the conditions that make an exoplanet habitable. Students evaluate evidence to predict which exoplanets might harbour life. Each group of two or three students will need 1 copy of the pupil worksheet 1 copy of the Planet profile to complete 1 copy of the sheet Habitable or not? to complete One Exoplanet information sheet. There are twelve of these, each about a different exoplanet. Each group needs a different one. They are best printed in colour and laminated. www.oxfordsparks.net/planet Possible Lesson Activities 1. Starter activity Show the animation ‘Rogue planet’ to the class. Repeat the viewing, focusing on the section on exoplanets from 1:32 to 2:16. 2. Main activity Divide the class into twelve groups, and outline the activity as described on the pupil worksheet. Allow students time to read Conditions for life and Habitable zone on the pupil worksheet, then check their understanding. Make the link between the term Goldilocks zone and the children’s story of the same name. Give each group one copy of the Planet profile proforma to complete as well as one Exoplanet information sheet. There are twelve Exoplanet information sheets; each group needs a different one. Allow time for each group to complete its Planet profile, then display these around the room.
    [Show full text]
  • Recent Results from Gravitational Microlensing
    Recent Results from Gravitational Microlensing • Bound planets • Unbound/Distant planets Takahiro Sumi (Osaka University) MOA collaboration NASA/JPL-Caltech/R. Hurt planetary microlensing Microlensing observation global network Survey Group Micro Follow-up Group lensing Alert MOA(NewZealand) PLANET µFUN OGLE(Chile), Robonet-II Anomaly Wide field Alert MiNDSTEp Low cadence • Pointing each candidate • High cadence MOA (since 1995) （Microlensing Observation in Astrophysics） （ New Zealand/Mt. John Observatory, Latitude： 44°S, Alt: 1029m ） Mirror : 1.8m CCD : 80M pix.(12x15cm) FOV : 2.2 deg.2 (10 times as full moon) Observational fields • 50 deg.2 disk Galactic Center • （２００x full moon） • ５0 M stars 1obs/１hr 1obs/１０min. ~600events／yr http://www.massey.ac.nz/~iabond/alert/alert.html Mass measurement of the cold, low-mass planet MOA-2009-BLG-266Lb Muraki et al. 2011 mp = 10.4 +- 1.7 MEarth M* = 0.56 +- 0.09 M a = 3.2 (+1.9 -0.5) AU Orbital period: P=7.6 (+7.7-1.5) yrs. demonstrates the capability to measure microlensing parallax with the Deep Impact (or EPOXI) spacecraft in a Heliocentric orbit. anomaly Summary of Planet candidates • RV • Transit (Kepler) • Direct image • Microlensing：14planets Mass measurements Mass by Bayesian Planet Frequency vs semimajor axis 6planets dN = 0.36 dex"2 dlogq dlogs M~0.5M 7x • Most ice & gas giant planets do not migrate very far in K,M dwarf ! dN/dloga=0.39±0.15 • Amount of migration M~M is a continuous parameter Gould et al. 2010 Planet mass ratio function 4 Neptune, 1 sub-Saturn, dN n "q 5 Jupiter dlogq n = −0.68 ±0.20 (Sumi et al.
    [Show full text]
  • Dust in Brown Dwarfs and Extrasolar Planets V
    A&A 603, A123 (2017) Astronomy DOI: 10.1051/0004-6361/201629696 & c ESO 2017 Astrophysics Dust in brown dwarfs and extrasolar planets V. Cloud formation in carbon- and oxygen-rich environments Ch. Helling, D. Tootill, P. Woitke, and G. Lee Centre for Exoplanet Science, SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY16 9SS, UK e-mail: [email protected] Received 12 September 2016 / Accepted 6 December 2016 ABSTRACT Context. Recent observations indicate potentially carbon-rich (C/O > 1) exoplanet atmospheres. Spectral fitting methods for brown dwarfs and exoplanets have invoked the C/O ratio as additional parameter but carbon-rich cloud formation modeling is a challenge for the models applied. The determination of the habitable zone for exoplanets requires the treatment of cloud formation in chemically different regimes. Aims. We aim to model cloud formation processes for carbon-rich exoplanetary atmospheres. Disk models show that carbon-rich or near-carbon-rich niches may emerge and cool carbon planets may trace these particular stages of planetary evolution. Methods. We extended our kinetic cloud formation model by including carbon seed formation and the formation of C[s], TiC[s], SiC[s], KCl[s], and MgS[s] by gas-surface reactions. We solved a system of dust moment equations and element conservation for a prescribed Drift-Phoenix atmosphere structure to study how a cloud structure would change with changing initial C/O0 = 0:43 ::: 10:0. Results. The seed formation efficiency is lower in carbon-rich atmospheres than in oxygen-rich gases because carbon is a very effective growth species.
    [Show full text]
  • Habitable Environments in Late Stellar Evolution
    Habitable Environments in Late Stellar Evolution Conditions for Abiogenesis in the Planetary Systems of White Dwarfs Author: Dewy Peters Supervisor: Prof. dr. F.F.S. van der Tak A thesis submitted in fulfillment of the requirements for the degree BSc in Astronomy Faculty of Science and Engineering University of Groningen The Netherlands March 2021 Abstract With very high potential transit-depths and an absence of stellar flare activity, the planets of White Dwarfs (WDs) are some of the most promising in the search for detectable life. Whilst planets with Earth-like masses and radii have yet to be detected around WDs, there is considerable evidence from spectroscopic and photometric observations that both terrestrial and gas-giant planets are capable of surviving post-main sequence evolution and migrating into the WD phase. WDs are also capable of hosting stable Habitable Zones outside orbital distances at which Earth-mass plan- ets would be disintegrated by tidal forces. Whilst transition- ing to the WD Phase, a main-sequence star has to progress along the Asymptotic Giant Branch (AGB), whereby orbit- ing planets would be subjected to atmospheric erosion by its harsh stellar winds. As a trade-off, the Circumstellar En- velope (CSE) of an AGB star is found to be rich in organics and some of the simple molecules from which more complex prebiotic molecules such as amino acids and simple sugars can be synthesised. It is found that planets with initial or- bital distances equivalent to those of Saturn and the Kuiper Belt would be capable of accreting a mass between 1 and 20 times that of the Earth’s atmosphere from the CSE and as a result, could obtain much of the material necessary to sustain life after the AGB and also experience minimal at- mospheric erosion.
    [Show full text]
  • Issue 117, March 2009
    NNASA’sASA’s LunarLunar ScienceScience InstituteInstitute BeginsBegins WorkWork It has been 40 years since humans fi rst set foot upon the Moon, taking that historic “giant step” for mankind. Although interest in our nearest celestial neighbor has waned considerably, it has never disappeared completely and is now enjoying a remarkable resurgence. The Moon was born when our home planet encountered a rogue planet at its birth, and has since recorded the earliest history of the solar system (a record nearly obliterated on Earth). With four spacecraft orbiting the Moon in the past three years (from four separate nation groups) and a fi fth, Lunar Reconnaissance Orbiter, due to arrive this spring, we are about to remake our understanding of this planetary body. To further contribute to the advancement of our knowledge, NASA recently created a Lunar Science Institute (NLSI) to revitalize the lunar science community and train a new generation of scientists. This spring, NASA has selected seven academic and research teams to form the initial core of the NLSI. This virtual institute is designed to support scientifi c research that supplements and extends existing NASA lunar science programs in coordination with U.S. space exploration policy. The new teams that augment NLSI were selected in a competitive evaluation process that began with the release of a cooperative agreement notice in June 2008. NASA received proposals from 33 research teams. L“We are extremely pleased with the response of the science community and the high quality of proposals received,” said David Morrison, the institute’s interim director at NASA Ames Research Center in Moffett Field, California.
    [Show full text]
  • Determining the True Mass of Radial-Velocity Exoplanets with Gaia F
    Determining the true mass of radial-velocity exoplanets with Gaia F. Kiefer, G. Hébrard, A. Lecavelier Des Etangs, E. Martioli, S. Dalal, A. Vidal-Madjar To cite this version: F. Kiefer, G. Hébrard, A. Lecavelier Des Etangs, E. Martioli, S. Dalal, et al.. Determining the true mass of radial-velocity exoplanets with Gaia: Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets. Astronomy and Astrophysics - A&A, EDP Sciences, 2021, 645, pp.A7. 10.1051/0004-6361/202039168. hal-03085694 HAL Id: hal-03085694 https://hal.archives-ouvertes.fr/hal-03085694 Submitted on 21 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 645, A7 (2021) Astronomy https://doi.org/10.1051/0004-6361/202039168 & © F. Kiefer et al. 2020 Astrophysics Determining the true mass of radial-velocity exoplanets with Gaia Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets? F. Kiefer1,2, G. Hébrard1,3, A. Lecavelier des Etangs1, E. Martioli1,4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne
    [Show full text]