DOCSLIB.ORG

September 2020 Newsletter for the Wiltshire, Swindon, Welcome to the New Season Beckington Astronomical Societies with the Pandemic Refusing to Go Away the Thing

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
September 2020 Newsletter for the Wiltshire, Swindon, Welcome to the New Season Beckington Astronomical Societies with the Pandemic Refusing to Go Away the Thing Volume26 Issue 1 NWASNEWS September 2020 Newsletter for the Wiltshire, Swindon, Welcome to the New Season Beckington Astronomical Societies With the pandemic refusing to go away the thing. Simon has looked at ways of col- committee having been discussing our lecting on line within our website, and Wiltshire Society Page 2 options going forward as safely as it is Bob Johnstone will accept cheques so possible, and this means our hall meetings we need to finalise details and we will Swindon Stargazers 3 will be postponed until at least January be in touch. Meanwhile be free to join us 2021, and even then we must be prepared on our web site and at Zoom session Beckington AS and Star Quest Astrono- 4 to move to alternative on line meetings that will be advertised. my Group page. until we feel it suitable to move back to We will continue with Zoom meetings rather SPACE NEWS 4-14 normal. This also applies to outreach and than hall meetings. See below for the Sep- 1960s Satellite returns to Earth observing sessions. tember Zoom Meeting ID and Password. Astronomers find 100 close by Brown Dwarfs Some other items that will need consensus Andy Burns is inviting you to a sched- Comet Neowise Spiraling as it passed from the members: uled Zoom meeting. Did a Supernova cause Mass Extinction No Chemical Difference between Our AGM will be on hold, because live Topic: Wiltshire AS September Meeting planetless stars. questions will be difficult to do if the Hubble took pictures of Neowise committee member is not available on Time: Sep 1, 2020 07:45 PM London First Daylight Laser Space Debris De- Zoom. tection Join Zoom Meeting I will stay on in position of chair while the Sun might have had a Companion. https://us02web.zoom.us/j/88178237251? Don Arabian dies. situation continues, again very difficult Did Betelgeuse Sneeze? to hand over without breaking social pwd=ckYzUDhNRjA0SnRUTUNZRVVqclZ distancing in this period, and it will aid QZz09 continuity. Members Logs, images and notes 14-15 Meeting ID: 881 7823 7251 FEES. We do not collect money for Passcode: 011090 What’s Up September 2020 16 Zoom meetings, but we do have back- ground costs that will need to be cov- Constellation of the Month: ered by an annual fee, and we have Aquarius 17-18 Keep good health... been looking at ways to collect these Clear skies Andy Burns. Space Station Timings 19 full in the knowledge that our bank, Lloyds, are very slow to change any- IMAGES, VIEWING SESSIONS and 20 OUTREACH The summer comet. Neowise F8 2020 This was taken after a session taking the comet in the evening of 20th July at the All Cannings Longbarrow. I was walking back to the VW and there was the com- et, perfectly framed over the By way . Quickly swapped to a 300mm lens on tripod. Andy Page 2 Volume25, Issue9 Wiltshire Society Page Membership Meeting nights £1.00 for members £3 for visitors Wiltshire Astronomical Society Wiltshire AS Contacts Web site: www.wasnet.org.uk Andy Burns Chair, [email protected] Facebook members page: https:// Andy Burns Outreach and newsletter editor. www.facebook.com/groups/ Bob Johnston (Treasurer) Debbie Croker (vice Treasurer) wiltshire.astro.society/ Philip Proven (Hall coordinator) Dave Buckle (Teas) Meetings 2020/2021. Peter Chappell (Speaker secretary) During COVID19 ZOOM meetingd Nick Howes (Technical Guru) Observing Sessions coordinators: Chris Brooks, Jon Gale, HALL VENUE the Pavilion, Rusty Lane, Seend Web coordinator: Sam Franklin Contact via the web site details. Meet 7.30 for 8.00pm start SEASON 2020/21 1 Sep Nick Howes/How do you solve a problem like debris-Ahh? Rusty Lane, Pavilion 6 Oct Martin Griffiths/The Big Bang, Evidence & Estiblishment 3 Nov Andrew Lound/A Jupiter Odyssey 1 Dec Dr Lilian Hobbs/Eisa Eisinga: The Planetarium in the Bedroom. 2021 5 Jan Open Forum/Beginner meeting. 2 Feb Prof David Southwood/Moon and Mars the next Giant Leap. 2 Mar Pete Williamson/The moon & Moons of the Solar System. 6 Apr Prof Mike Edmunds/The Clockwork universe. 4 May TBC 1 Jun Robert Harvey/Understanding the Universe. Thank you Peter and those that have helped get a list together in the circumstances. Observing Sessions see back page Nick Howes We are all finding problems with the space being filled with constellations of thousands of satellites being launched into Low Earth Orbit. Now what about all the broken pieces, redundant satel- lites and even secondary launch debris? And how do you launch new missions through this mess? Nick Howes, our technical committee member is now en- gaged with the British programme of space launches had has a first hand perspective on the problem. Page 3 Swindon’s own astronomy group Meeting Dates for 2020 -------Summer Break------ Meetings cancelled Friday 18 September Due to the current crisis our meetings, like many oth- Programme: AGM if restrictions lifted. ers have been cancelled at least until after the summer Friday 16 October break. We hope to reconvene again in September when the postponed AGM will be held. Programme: Dr James Fradgley MSc, FRAS: The Universe - 'A brief overview of what we know, or think Ad-hoc viewing sessions postponed we know' All ad-hoc meetings are currently cancelled until fur- Friday 20 November ther notice. Programme: Dave Eagle FRAS PGCE BSc (Hons): Regular stargazing evenings are being organised near 'Comets, Enigmatic and Beautiful Visitors' Swindon. To join these events please visit our website for further information. Lately we have been stargazing at Blakehill Farm Na- ture Reserve near Cricklade, a very good spot with no distractions from car headlights. Website: We often meet regularly at a lay-by just outside the village of Uffcott, near Wroughton. Directions are also http://www.swindonstargazers.com shown on the website link below. Information about our evenings and viewing spots can Chairman: Robin Wilkey be found here: Tel No: 07808 775630 http://www.swindonstargazers.com/noticeboard/ Email: [email protected] noticeboard06.htm Address: 61 Northern Road Swindon, SN2 1PD For insurance reasons you need to be a club member to take part. If you think you might be interested email the organiser Secretary: Hilary Wilkey Robin Wilkey (see below). With this you will then be emailed regarding the event, whether it is going ahead Tel No: 01793 574403 or whether it will be cancelled because of cloud etc. Email: [email protected] Address: 61 Northern Road We are a small keen group and I would ask you to note that you DO NOT have to own a telescope to take Swindon, SN2 1PD part, just turn up and have a great evening looking through other people's scopes. We are out there to share an interest and the hobby. There's nothing better than practical astronomy in the great cold British win- ter! And hot drinks are often available, you can also bring your own. Enjoy astronomy at it's best! Meetings at Liddington Village Hall, Church Road, Liddington, SN4 0HB – 7.30pm onwards The hall has easy access from Junction 15 of the M4, a map and directions can be found on our website at: http://www.swindonstargazers.com/clubdiary/ directions01.htm Page 4 BECKINGTON ASTRONOMICAL SOCIETY SPACE NEWS FOR SEPTEMBER 2020 Society Details & Speakers programme can be found on our Website www.beckingtonas.org General enquiries about the Society can be emailed to chair- [email protected]. Long retired Satellite falls to Earth Our Committee for 2016/2017 is © Provided by Space NASA's Orbiting Geophysical Obser- Chairman: Steve Hill (email [email protected]) vatory 1, or OGO-1, is seen in orbit on Aug. 25, 2020. The Treasurer: John Ball satellite launched in September 1964 and fell to Earth on Secretary: Sandy Whitton Aug. 29, 2020. Ordinary Member: Mike Witt A long-retired NASA satellite burned up in Earth's atmos- phere over the weekend, the agency has confirmed. People can find out more about us at www.beckingtonas.org NASA launched the satellite, called Orbiting Geophysics Meetings take place in Beckington Baptist Church Hall in Observatory 1, or OGO-1, in September 1964, the first in a Beckington Village near Frome. series of five missions to help scientists understand the magnetic environment around Earth. OGO-1 was the first to See the location page for details of how to find us on our web- launch but the last to fall out of orbit; the satellite had cir- site………… cled Earth aimlessly since its retirement in 1971. Post Code for Sat Nav is BA11 6TB. But orbiting Earth is a tricky thing to do, since the particles Our start time is 7.30pm in our plush atmosphere collide with spacecraft and slow them down, even at very high altitudes where the atmos- phere is thin. That speed reduction also lowers the space- craft's altitude, until reentry becomes inevitable. Date Title Speaker Related: The biggest spacecraft ever to fall uncon- trolled from space th 19 June To Be Informed The 1,070-lb. (487 kilograms) OGO-1 experienced that inevitability on Saturday (Aug. 29), as NASA had predicted. The satellite re-entered at 4:44 p.m. EDT (2044 GMT) over the southern Pacific Ocean and burned up in the atmos- phere, posing no threat to humans, NASA spokesperson Josh Handal told Space.com in an email. The spacecraft hit the atmosphere about 25 minutes earlier This young astronomy club meets at the than NASA had forecast, Handal said, resulting in a reentry Sutton Veny Village Hall. location east of the agency's predictions. OGO-1 re-entered about 100 miles (160 kilometers) southeast of Tahiti, he Second Thursday of the Month.
Load more

Recommended publications
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • Simulating (Sub)Millimeter Observations of Exoplanet Atmospheres in Search of Water
    University of Groningen Kapteyn Astronomical Institute Simulating (Sub)Millimeter Observations of Exoplanet Atmospheres in Search of Water September 5, 2018 Author: N.O. Oberg Supervisor: Prof. Dr. F.F.S. van der Tak Abstract Context: Spectroscopic characterization of exoplanetary atmospheres is a field still in its in- fancy. The detection of molecular spectral features in the atmosphere of several hot-Jupiters and hot-Neptunes has led to the preliminary identification of atmospheric H2O. The Atacama Large Millimiter/Submillimeter Array is particularly well suited in the search for extraterrestrial water, considering its wavelength coverage, sensitivity, resolving power and spectral resolution. Aims: Our aim is to determine the detectability of various spectroscopic signatures of H2O in the (sub)millimeter by a range of current and future observatories and the suitability of (sub)millimeter astronomy for the detection and characterization of exoplanets. Methods: We have created an atmospheric modeling framework based on the HAPI radiative transfer code. We have generated planetary spectra in the (sub)millimeter regime, covering a wide variety of possible exoplanet properties and atmospheric compositions. We have set limits on the detectability of these spectral features and of the planets themselves with emphasis on ALMA. We estimate the capabilities required to study exoplanet atmospheres directly in the (sub)millimeter by using a custom sensitivity calculator. Results: Even trace abundances of atmospheric water vapor can cause high-contrast spectral ab- sorption features in (sub)millimeter transmission spectra of exoplanets, however stellar (sub) millime- ter brightness is insufficient for transit spectroscopy with modern instruments. Excess stellar (sub) millimeter emission due to activity is unlikely to significantly enhance the detectability of planets in transit except in select pre-main-sequence stars.
    [Show full text]
  • What Can the Dispersed Matter Planet Project Do for ARIEL?
    What can the Dispersed Matter Planet Project do for ARIEL? Carole Haswell, The Open University Principal Collaborators: Dan Staab, John Barnes, Luca Fossati, MarK Jones, GuilleM Angelada-Escude, JaMes Doherty, Joe Cooper, JaMes Jenkins Outline • motivation: WASP-12: stellar activity masked by planetary mass loss new way to select host stars of ablating planets • Dispersed Matter Planet Project (DMPP) Search for Them among BRIGHT NEARBY STARS! Very efficient RV planet search 39 initial targets, good success rate • First discoveries DMPP-1, DMPP-2, DMPP-3 … • Characterisation of DMPP planets mass-radius-composition relationships, exogeology • DMPP systems good for characterisation even if not transiting… Activity: characterised by RHK Line core Emission strength Fossati, Ayres, Haswell, Bohlender, Kochukhov & Floer 2013, ApJLett Ca II H& K line cores Activity: characterised by RHK Line core emission quenched by diffuse gas Dan Staab PhD work Haswell, Staab, Barnes, Anglada-Escude, Fossati, Jenkins, Norton, Doherty, Cooper 2019, Nature Astronomy arXiv:1912.10874 Activity: characterised by RHK > 40% of close-in planet hosts: depressed CaII H&K OU-SALT survey Doherty, Haswell, Barnes, Staab, Fossati 2018, Poster Cool Stars 20; 2019 in prep Staab, Haswell, Smith, Fossati, Barnes, Busuttil, Jenkins, MNRAS, 2017, 466, 738 Absorbing gas constrained to orbital plane? Haswell, Fossati, Ayres, France, Froning et al 2012, ApJ, 760, 79 Mass-losing Close-in planets e.g. Kepler 1520b have HUGE sCale-heights KIC 1255b aka Kepler 1520b: • DeteCted by transiting
    [Show full text]
  • Open Batalha-Dissertation.Pdf
    The Pennsylvania State University The Graduate School Eberly College of Science A SYNERGISTIC APPROACH TO INTERPRETING PLANETARY ATMOSPHERES A Dissertation in Astronomy and Astrophysics by Natasha E. Batalha © 2017 Natasha E. Batalha Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2017 The dissertation of Natasha E. Batalha was reviewed and approved∗ by the following: Steinn Sigurdsson Professor of Astronomy and Astrophysics Dissertation Co-Advisor, Co-Chair of Committee James Kasting Professor of Geosciences Dissertation Co-Advisor, Co-Chair of Committee Jason Wright Professor of Astronomy and Astrophysics Eric Ford Professor of Astronomy and Astrophysics Chris Forest Professor of Meteorology Avi Mandell NASA Goddard Space Flight Center, Research Scientist Special Signatory Michael Eracleous Professor of Astronomy and Astrophysics Graduate Program Chair ∗Signatures are on file in the Graduate School. ii Abstract We will soon have the technological capability to measure the atmospheric compo- sition of temperate Earth-sized planets orbiting nearby stars. Interpreting these atmospheric signals poses a new challenge to planetary science. In contrast to jovian-like atmospheres, whose bulk compositions consist of hydrogen and helium, terrestrial planet atmospheres are likely comprised of high mean molecular weight secondary atmospheres, which have gone through a high degree of evolution. For example, present-day Mars has a frozen surface with a thin tenuous atmosphere, but 4 billion years ago it may have been warmed by a thick greenhouse atmosphere. Several processes contribute to a planet’s atmospheric evolution: stellar evolution, geological processes, atmospheric escape, biology, etc. Each of these individual processes affects the planetary system as a whole and therefore they all must be considered in the modeling of terrestrial planets.
    [Show full text]
  • Institute of Astrophysics and Space Sciences 2018 Activity Report
    Institute of Astrophysics and Space Sciences 2018 Activity Report Institute of Astrophysics and Space Sciences 2018 Activity Report COFINANCIAMENTO 2018 IA ACTIVITY REPORT | 3 ​ ​ Index Unit Overview 5 IA Management 6 Visitor Program at the Institute for Astrophysics and Space Sciences 7 Incentive Program for the Training of Excellence of Young Researchers in Astrophysics and Space Sciences 7 IA-ON 5 8 The IA team (2018) 9 Origin and Evolution of Stars and Planets Group 9 Galaxies, Cosmology, and the Evolution of the Universe Group 10 Instrumentation and Systems Group 11 Interface to Science 11 ​ ​ Research Projects/Programmes 12 ​ Projects focused on scientific activities 12 ​ ​ Projects focused on communication and outreach 15 ​ ​ Scientific Output and Activities 16 Origin and Evolution of Stars and Planets 20 Towards the detection and characterisation of other Earths 21 Towards a comprehensive study of stars 25 Galaxies, Cosmology, and the Evolution of the Universe 30 The assembly history of galaxies resolved in space and time 32 Unveiling the dynamics of the Universe 36 Instrumentation and Systems 39 Space and Ground Systems and Technologies 45 Science Communication 47 The Portuguese ALMA Centre of Expertise 50 Scientific Output 53 Books 53 Published articles 53 Book chapters and Proceedings 59 Book chapters and Proceedings 59 International Scientific Communications 61 National Scientific Communications 65 Organization of Conferences 55 Seminars at IA 66 Organization of Conferences 67 Observing runs 67 Outreach talks 69 4 | IA ACTIVITY REPORT 2018 ​ ​ Reports 72 External seminars by IA researchers 72 PhD completed 73 MSc Projects completed 74 BSc Traineeships/Projects completed 74 2018 IA ACTIVITY REPORT | 5 ​ ​ Unit Overview The Instituto de Astrofísica e Ciências do Espaço (IA) is the reference institution for research in ​ ​ Astronomy, Astrophysics and Space Sciences in Portugal, implementing a bold strategy for the development of this area in the country.
    [Show full text]
  • AMD-Stability and the Classification of Planetary Systems
    A&A 605, A72 (2017) DOI: 10.1051/0004-6361/201630022 Astronomy c ESO 2017 Astrophysics& AMD-stability and the classification of planetary systems? J. Laskar and A. C. Petit ASD/IMCCE, CNRS-UMR 8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 7 November 2016 / Accepted 23 January 2017 ABSTRACT We present here in full detail the evolution of the angular momentum deficit (AMD) during collisions as it was described in Laskar (2000, Phys. Rev. Lett., 84, 3240). Since then, the AMD has been revealed to be a key parameter for the understanding of the outcome of planetary formation models. We define here the AMD-stability criterion that can be easily verified on a newly discovered planetary system. We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit the planetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require some additional dynamical studies to conclude on their stability. The AMD-stability classification is applied to the 131 multiplanet systems from The Extrasolar Planet Encyclopaedia database for which the orbital elements are sufficiently well known. Key words. chaos – celestial mechanics – planets and satellites: dynamical evolution and stability – planets and satellites: formation – planets and satellites: general 1. Introduction motion resonances (MMR, Wisdom 1980; Deck et al. 2013; Ramos et al. 2015) could justify the Hill-type criteria, but the The increasing number of planetary systems has made it nec- results on the overlap of the MMR island are valid only for close essary to search for a possible classification of these planetary orbits and for short-term stability.
    [Show full text]
  • Planets and Exoplanets
    NASE Publications Planets and exoplanets Planets and exoplanets Rosa M. Ros, Hans Deeg International Astronomical Union, Technical University of Catalonia (Spain), Instituto de Astrofísica de Canarias and University of La Laguna (Spain) Summary This workshop provides a series of activities to compare the many observed properties (such as size, distances, orbital speeds and escape velocities) of the planets in our Solar System. Each section provides context to various planetary data tables by providing demonstrations or calculations to contrast the properties of the planets, giving the students a concrete sense for what the data mean. At present, several methods are used to find exoplanets, more or less indirectly. It has been possible to detect nearly 4000 planets, and about 500 systems with multiple planets. Objetives - Understand what the numerical values in the Solar Sytem summary data table mean. - Understand the main characteristics of extrasolar planetary systems by comparing their properties to the orbital system of Jupiter and its Galilean satellites. The Solar System By creating scale models of the Solar System, the students will compare the different planetary parameters. To perform these activities, we will use the data in Table 1. Planets Diameter (km) Distance to Sun (km) Sun 1 392 000 Mercury 4 878 57.9 106 Venus 12 180 108.3 106 Earth 12 756 149.7 106 Marte 6 760 228.1 106 Jupiter 142 800 778.7 106 Saturn 120 000 1 430.1 106 Uranus 50 000 2 876.5 106 Neptune 49 000 4 506.6 106 Table 1: Data of the Solar System bodies In all cases, the main goal of the model is to make the data understandable.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
    exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD
    [Show full text]
  • The Stability of Ultra-Compact Planetary Systems
    A&A 516, A82 (2010) Astronomy DOI: 10.1051/0004-6361/200912698 & c ESO 2010 Astrophysics The stability of ultra-compact planetary systems B. Funk1, G. Wuchterl2,R.Schwarz1,3, E. Pilat-Lohinger3, and S. Eggl3 1 Department of Astronomy, Eötvös Loránd University, Pázmány Péter Sétány 1/A, 1117 Budapest, Hungary e-mail: [email protected] 2 Thüringer Landessternwarte, Sternwarte 5, 07778 Tautenburg, Germany e-mail: [email protected] 3 Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria e-mail: [schwarz;lohinger;eggl]@astro.univie.ac.at Received 15 June 2009 / Accepted 15 March 2010 ABSTRACT Aims. We investigate the dynamical stability of compact planetary systems in the CoRoT discovery space, i.e., with orbital periods of less than 50 days, including a detailed study of the stability of systems, which are spaced according to Hill’s criteria. Methods. The innermost fictitious planet was placed close to the Roche limit from the star (MStar = 1 MSun) and all other fictitious planets are lined up according to Hill’s criteria up to a distance of 0.26 AU, which corresponds to a 50 day period for a Sun-massed star. For the masses of the fictitious planets, we chose a range of 0.33–17 mEarth, where in each simulation all fictitious planets have the same mass. Additionally, we tested the influence of both the semi-major axis of the innermost planet and of the number of planets. In a next step we also included a gas giant in our calculations, which perturbs the inner ones and investigated their stability.
    [Show full text]
  • The TRAPPIST-1 JWST Community Initiative
    Bulletin of the AAS • Vol. 52, Issue 2 The TRAPPIST-1 JWST Community Initiative Michaël Gillon1, Victoria Meadows2, Eric Agol2, Adam J. Burgasser3, Drake Deming4, René Doyon5, Jonathan Fortney6, Laura Kreidberg7, James Owen8, Franck Selsis9, Julien de Wit10, Jacob Lustig-Yaeger11, Benjamin V. Rackham10 1Astrobiology Research Unit, University of Liège, Belgium, 2Department of Astronomy, University of Washington, USA, 3Department of Physics, University of California San Diego, USA, 4Department of Astronomy, University of Maryland at College Park, USA, 5Institute for Research in Exoplanets, University of Montreal, Canada, 6Other Worlds Laboratory, University of California Santa Cruz, USA, 7Center for Astrophysics | Harvard and Smithsonian, USA, 8Department of Physics, Imperial College London, United Kingdom, 9Laboratoire d’Astrophysique de Bordeaux, University of Bordeaux, France, 10Department of Earth, Atmospheric, and Planetary Sciences, MIT, USA, 11Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA Published on: Dec 02, 2020 DOI: 10.3847/25c2cfeb.afbf0205 License: Creative Commons Attribution 4.0 International License (CC-BY 4.0) Bulletin of the AAS • Vol. 52, Issue 2 The TRAPPIST-1 JWST Community Initiative ABSTRACT The upcoming launch of the James Webb Space Telescope (JWST) combined with the unique features of the TRAPPIST-1 planetary system should enable the young field of exoplanetology to enter into the realm of temperate Earth-sized worlds. Indeed, the proximity of the system (12pc) and the small size (0.12 R )
    [Show full text]
  • El Sistema Planetario De Trappist-1
    (#313). EL SISTEMA PLANETARIO DE TRAPPIST-1 [MONOTEMA] El descubrimiento del sistema TRAPPIST-1 ha generado gran interés debido, fundamentalmente, a que los siete planetas detectados tienen características similares a la Tierra y podrían albergar vida. Esos planetas orbitan alrededor de una estrella enana tipo M, y además lo hacen de manera resonante y con acoplamiento por fuerzas de marea. En este post describo los detalles más relevantes de este hallazgo, y explico de forma breve los principales métodos de detección empleados en este campo de la física, así como también analizo la posible habitabilidad de los planetas encontrados. Muestro, por tanto, de manera didáctica, la complejidad de obtener resultados concluyentes cuando todavía existe incertidumbre importante en los datos, pero al mismo tiempo ilustro que a través de la observación, simulación numérica y análisis estadísticos, se puede obtener un dibujo aproximado de una parte de la galaxia que está a unos 39 años luz de nosotros. Introducción El descubrimiento de tres exoplanetas en la zona habitable de la estrella TRAPPIST-1A por Gillon et al. (2016), ha sido uno de los eventos más destacados en el campo de la astrofísica en los últimos años. Tan sólo unos meses más tarde, Gillon et al. (2017) publicaron que habían detectado hasta 7 planetas orbitando esa estrella, los cuales podrían contener agua líquida. De este modo, el hallazgo de los exoplanetas de TRAPPIST-1 constituye un caso muy atractivo para ilustrar algunas de las actividades fundamentales de la investigación en astrofísica, así como para explicar conceptos clave asociados a la búsqueda de lugares en el espacio con el potencial de albergar vida.
    [Show full text]
  • 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
    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 Université, CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France e-mail: [email protected] 2 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France 3 Observatoire de Haute-Provence, CNRS, Université d’Aix-Marseille, 04870 Saint-Michel-l’Observatoire, France 4 Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, 37504-364, Itajubá - MG, Brazil Received 12 August 2020 / Accepted 24 September 2020 ABSTRACT Mass is one of the most important parameters for determining the true nature of an astronomical object. Yet, many published exoplanets lack a measurement of their true mass, in particular those detected as a result of radial-velocity (RV) variations of their host star. For those examples, only the minimum mass, or m sin i, is known, owing to the insensitivity of RVs to the inclination of the detected orbit compared to the plane of the sky. The mass that is given in databases is generally that of an assumed edge-on system ( 90◦), but many ∼ other inclinations are possible, even extreme values closer to 0◦ (face-on). In such a case, the mass of the published object could be strongly underestimated by up to two orders of magnitude.
    [Show full text]