DOCSLIB.ORG

2550 (Created: Tuesday, March 30, 2021 at 7:23:07 PM Eastern Standard Time) - Overview

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
2550 (Created: Tuesday, March 30, 2021 at 7:23:07 PM Eastern Standard Time) - Overview JWST Proposal 2550 (Created: Tuesday, March 30, 2021 at 7:23:07 PM Eastern Standard Time) - Overview 2550 - The First Near-IR Spectroscopic Survey of Neptune Trojans Cycle: 1, Proposal Category: GO INVESTIGATORS Name Institution E-Mail Larissa Markwardt (PI) University of Michigan [email protected] Dr. Hsing Wen Lin (CoI) University of Michigan [email protected] Prof. David Gerdes (CoI) University of Michigan [email protected] Prof. Renu Malhotra (CoI) University of Arizona [email protected] Kevin Napier (CoI) University of Michigan [email protected] Dr. Fred Adams (CoI) University of Michigan [email protected] OBSERVATIONS Folder Observation Label Observing Template Science Target Observation Folder 1 NIRSpec IFU:2008 LC NIRSpec IFU Spectroscopy (2) 2008LC18 18 3 NIRSpec IFU: 2011 W NIRSpec IFU Spectroscopy (6) 2011WG157 G157 5 NIRSpec IFU: 2013 K NIRSpec IFU Spectroscopy (4) 2013KY18 Y18 7 NIRSpec IFU: 2011 H NIRSpec IFU Spectroscopy (3) 2011HM102 M102 10 NIRSpec IFU: 2013 V NIRSpec IFU Spectroscopy (5) 2013VX30 X30 11 NIRSpec IFU: 2006 RJ NIRSpec IFU Spectroscopy (12) 2006RJ103 103 12 NIRSpec IFU: 2007 VL NIRSpec IFU Spectroscopy (8) 2007VL305 305 1 JWST Proposal 2550 (Created: Tuesday, March 30, 2021 at 7:23:07 PM Eastern Standard Time) - Overview Folder Observation Label Observing Template Science Target 13 NIRSpec IFU: 2011 SO NIRSpec IFU Spectroscopy (7) 2011SO277 277 14 NIRSpec IFU: 2010 TS NIRSpec IFU Spectroscopy (11) 2010TS191 191 ABSTRACT Trojan asteroids, which librate around a planet’s L4 or L5 point, are thought to be remnants of our primordial disk as the strong 1:1 resonance means they can be stable on order the age of the Solar System. This resonance relationship means that Trojans are also tied to the evolution of their planet, meaning that giant planet Trojans can also be used to constrain planetary migration models. Neptune Trojans (NTs) are a particularly puzzling population; while they are expected to have a mix of red and ultra-red surfaces, only one ultra-red NT has been discovered to date. It is possible that collisions between NTs and Plutinos shifted the NT colors blueward over time, but colors are limited in their capacity to answer this question as a variety of processes and compositions can affect the colors of planetary bodies, often in ways that are indistinguishable from each other. Near-IR spectra can provide more information about these planetary surfaces as many broad molecular absorption features occur at these wavelengths. In particular, these features can be used to measure ice composition, ice irradiation products, surface grain size, and the ice phase. Therefore, we propose to take the first near-IR spectroscopic survey of NTs in order to study the ultra-red NT's surface in more detail, compare L4 and L5 NTs, and compare unstable NTs to Centaurs. JWST is vital to this program as these objects are too faint to take reasonable spectra using ground-based facilities. Regardless of the exact outcomes, these measurements would lead to a better understanding of the formation and evolution of NTs and the giant planets. OBSERVING DESCRIPTION The requested observations are to take Near-IR reflectance spectra of 9 Neptune Trojans. We will be using the NIRSpec IFU with the PRISM for all of the targets. We will not be doing any target aquisition, instead doing a blind pointing into the IFU FOV; the positional uncertainties for all of our targets + the pointing uncertainty will be less than 1.5" at the time of observation. We will also be using a 2-point nod dither pattern and the NRSIRS2RAPID readout pattern for all of our targets. All of our targets are distant Solar System objects, meaning they will be point sources and will not exceed the angular rate of motion limit. Our list of targets (with overall science time) is as follows: - 2008 LC18 - 3.24 hrs - 2011 WG157 -0.8 hrs - 2013 KY18 - 0.8 hrs - 2011 HM102 - 2 hrs 2 JWST Proposal 2550 (Created: Tuesday, March 30, 2021 at 7:23:07 PM Eastern Standard Time) - Overview - 2013 VX30 - 1 hrs - 2006 RJ103 - 0.8 hrs - 2007 VL305 - 1.2 hrs - 2011 SO277 - 1.2 hrs - 2010 TS191 - 1.6 hrs 3 Proposal 2550 - Targets - The First Near-IR Spectroscopic Survey of Neptune Trojans # Name Level 1 Level 2 Level 3 (2) 2008LC18 TYPE=ASTEROID,A=30.05039893570054,E=0.0795 6797229116722,I=27.50484015385932,O=88.5256719 5979223,W=4.899676951511355,M=169.8904076596 557,EQUINOX=J2000,EPOCH=31-AUG- 2009:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=Unknown (3) 2011HM102 TYPE=ASTEROID,A=30.09129189747453,E=0.0807 4695180988048,I=29.40338876077627,O=100.984958 8268076,W=150.8564999915705,M=29.76256592484 921,EQUINOX=J2000,EPOCH=30-AUG- 2015:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=NO (4) 2013KY18 TYPE=ASTEROID,A=30.09195046629077,E=0.1199 81181551389,I=6.666842318991241,O=84.379298024 64498,W=272.1220317711166,M=268.462456114411 8,EQUINOX=J2000,EPOCH=27-MAY- 2014:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=NO (5) 2013VX30 TYPE=ASTEROID,A=30.00653186954801,E=0.0815 3095417969938,I=31.31460868473241,O=192.592491 0907664,W=216.1479151673698,M=353.9481301936 667,EQUINOX=J2000,EPOCH=01-NOV- 2016:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=NO (6) 2011WG157 TYPE=ASTEROID,A=30.15115751243756,E=0.0248 0723477878031,I=22.30505410483727,O=352.197666 Solar System Targets 9383424,W=208.6267604521326,M=208.6821859568 394,EQUINOX=J2000,EPOCH=02-AUG- 2013:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=NO (7) 2011SO277 TYPE=ASTEROID,A=30.22265998181066,E=0.0091 30811445308824,I=9.639190126377523,O=113.62368 40528006,W=114.2219980449608,M=151.613414690 4316,EQUINOX=J2000,EPOCH=27-AUG- 2013:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=NO (8) 2007VL305 TYPE=ASTEROID,A=30.04056798197746,E=0.0635 9636971777168,I=28.14946912075748,O=188.681146 3176001,W=218.3894487958658,M=4.352123802605 181,EQUINOX=J2000,EPOCH=16-JUN- 2015:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=NO 4 Proposal 2550 - Targets - The First Near-IR Spectroscopic Survey of Neptune Trojans (11) 2010TS191 TYPE=ASTEROID,A=30.07317861653429,E=0.0485 0532908303209,I=6.562466790819702,O=129.685361 9331111,W=300.6148163643498,M=336.2465379252 896,EQUINOX=J2000,EPOCH=24-JUN- 2014:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=Unknown (12) 2006RJ103 TYPE=ASTEROID,A=30.04482399069547,E=0.0317 9587760688634,I=8.161556879320241,O=120.965271 3533018,W=25.53486982632182,M=253.7833917219 978,EQUINOX=J2000,EPOCH=25-DEC- 2014:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=Unknown 5 Proposal 2550 - Observation 1 - The First Near-IR Spectroscopic Survey of Neptune Trojans Proposal 2550, Observation 1: NIRSpec IFU:2008 LC18 Wed Mar 31 00:23:07 GMT 2021 Diagnostic Status: Warning Observing Template: NIRSpec IFU Spectroscopy Observation (Visit 1:1) Warning (Form): Overheads are provisional until the Visit Planner has been run. Diagnostics # Name Level 1 Level 2 Level 3 (2) 2008LC18 TYPE=ASTEROID,A=30.05039893570054,E=0.0795 6797229116722,I=27.50484015385932,O=88.5256719 5979223,W=4.899676951511355,M=169.8904076596 557,EQUINOX=J2000,EPOCH=31-AUG- 2009:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=Unknown Solar System Targets TA Method NONE Template # Dither Type Size Starting Point Number of Points Points 1 2-POINT-NOD Dithers # Grating/Filter Readout Groups/Int Integrations/Ex Leakcal Dither Autocal Total Dithers Total Total Exposure ETC Pattern p Integrations Time Wkbk.Calc ID 1 PRISM/CLEAR NRSIRS2RAPI 50 8 false true NONE 2 16 11904.534 61740 D Spectral Elements DEFAULT WINDOW: ANGULAR RATE 2008LC18 FROM JWST LESS THAN 0.03 Special Requirements 6 Proposal 2550 - Observation 3 - The First Near-IR Spectroscopic Survey of Neptune Trojans Proposal 2550, Observation 3: NIRSpec IFU: 2011 WG157 Wed Mar 31 00:23:07 GMT 2021 Diagnostic Status: Warning Observing Template: NIRSpec IFU Spectroscopy Observation (Visit 3:1) Warning (Form): Overheads are provisional until the Visit Planner has been run. Diagnostics # Name Level 1 Level 2 Level 3 (6) 2011WG157 TYPE=ASTEROID,A=30.15115751243756,E=0.0248 0723477878031,I=22.30505410483727,O=352.197666 9383424,W=208.6267604521326,M=208.6821859568 394,EQUINOX=J2000,EPOCH=02-AUG- 2013:00:00:00,EpochTimeScale=TDB Comments: Keyword=Asteroid Description=Neptune Trojan Extended=NO Solar System Targets TA Method NONE Template # Dither Type Size Starting Point Number of Points Points 1 2-POINT-NOD Dithers # Grating/Filter Readout Groups/Int Integrations/Ex Leakcal Dither Autocal Total Dithers Total Total Exposure ETC Pattern p Integrations Time Wkbk.Calc ID 1 PRISM/CLEAR NRSIRS2RAPI 50 2 false true NONE 2 4 2976.134 D Spectral Elements DEFAULT WINDOW: ANGULAR RATE 2011WG157 FROM JWST LESS THAN 0.03 Special Requirements 7 Proposal 2550 - Observation 5 - The First Near-IR Spectroscopic Survey of Neptune Trojans Proposal 2550, Observation 5: NIRSpec IFU: 2013 KY18 Wed Mar 31 00:23:07 GMT 2021 Diagnostic Status: Warning Observing Template: NIRSpec IFU Spectroscopy Observation (Visit 5:1) Warning (Form): Overheads are provisional until the Visit Planner has been run. Diagnostics # Name Level 1 Level 2 Level 3 (4) 2013KY18 TYPE=ASTEROID,A=30.09195046629077,E=0.1199 81181551389,I=6.666842318991241,O=84.379298024
Load more

Recommended publications
  • Joint Institute for VLBI in Europe Biennial Report 2011-2012
    Joint Institute For VLBI in Europe 11-12 Biennial report 2011-2012 The Joint Institute for VLBI in Europe (JIVE) was established as a scientific foundation in December 1993. JIVE’s mandate is to support the operations of the European VLBI Network (EVN) in the widest sense. JIVE’s operations are supported via multi‐national funds from the following organisations: Netherlands Institute for Radio Astronomy (ASTRON), the Netherlands, National Center for Scientific Research (CNRS), France National Geographical Institute (IGN), Spain, Italian National Institute of Astrophysics (INAF), Italy, Max Planck Institute for Radio Astronomy (MPIfR), Germany, National Astronomical Observatories of China (NAOC), China, National Research Foundation (NRF), South Africa Netherlands Organisation for Scientific Research (NWO), the Netherlands, Onsala Space Observatory (OSO), Sweden, Science & Technology Facilities Council (STFC), UK Joint Institute for VLBI in Europe | Biennial report 2011‐2012 Contents 1. INSTITUTE ....................................................................................................................................................... 1 1.1. preparing for the next funding cycle ..................................................................................................... 1 1.2. enhancing the VLBI capabilities ............................................................................................................. 2 1.3. JIVE events ............................................................................................................................................
    [Show full text]
  • The Size Distribution of the Neptune Trojans and the Missing Intermediate-Sized Planetesimals
    The Astrophysical Journal Letters, 723:L233–L237, 2010 November 10 doi:10.1088/2041-8205/723/2/L233 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE SIZE DISTRIBUTION OF THE NEPTUNE TROJANS AND THE MISSING INTERMEDIATE-SIZED PLANETESIMALS Scott S. Sheppard1 and Chadwick A. Trujillo2 1 Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Rd. NW, Washington, DC 20015, USA; [email protected] 2 Gemini Observatory, 670 North A’ohoku Place, Hilo, HI 96720, USA Received 2010 July 29; accepted 2010 September 29; published 2010 October 20 ABSTRACT We present an ultra-deep survey for Neptune Trojans using the Subaru 8.2 m and Magellan 6.5 m telescopes. 2 The survey reached a 50% detection efficiency in the R band at mR = 25.7 mag and covered 49 deg of sky. mR = 25.7 mag corresponds to Neptune Trojans that are about 16 km in radius (assuming an albedo of 0.05). A paucity of smaller Neptune Trojans (radii < 45 km) compared with larger ones was found. The brightest Neptune Trojans appear to follow a steep power-law slope (q = 5 ± 1) similar to the brightest objects in the other known stable reservoirs such as the Kuiper Belt, Jupiter Trojans, and main belt asteroids. We find a roll-over for the Neptune Trojans that occurs around a radius of r = 45 ± 10 km (mR = 23.5 ± 0.3), which is also very similar to the other stable reservoirs. All the observed stable regions in the solar system show evidence for Missing Intermediate-Sized Planetesimals (MISPs).
    [Show full text]
  • Trailing (L5) Neptune Trojans: 2004 KV18 and 2008 LC18
    Trailing (L5) Neptune Trojans: 2004 KV18 and 2008 LC18 Pu Guan, Li-Yong Zhou,∗ Jian Li Astronomy Department, Nanjing University, Key Laboratory of Modern Astronomy and Astrophysics in MOE, Nanjing 210093, China November 11, 2018 Abstract The population of Neptune Trojans is believed to be bigger than that of Jupiter Trojans and that of asteroids in the main belt, although only eight members of this far distant asteroid swarm have been observed up to now. Six leading Neptune Trojans around the Lagrange point L4 dis- covered earlier have been studied in detail, but two trailing ones found recently around the L5 point, 2004 KV18 and 2008 LC18, have not been investigated yet. In this paper, we report our investigations on the dynamical behaviors of these two new Neptune Trojans. Our calculations show that the asteroid 2004 KV18 is a temporary Neptune Trojan. Most probably, it was captured into the trailing Trojan cloud no earlier than 2.03 105 yr ago, and it will not keep this identity no later than 1.65 105 yr in future. Based on the× statistics on our orbital simulations, we argue that this object is more× like a scattered Kuiper belt object. On the contrary, the orbit of asteroid 2008 LC18 is much more stable. Among the clone orbits spread within the orbital uncertainties, a considerable portion of clones may survive on the L5 tadpole orbits for 4Gyr. The strong depen- dence of the stability on the semimajor axis and resonant angle suggests that further observations are badly needed to confine the orbit in the stable region.
    [Show full text]
  • Dr. Alex Harrison Parker Postdoctoral Fellow in Planetary Astronomy
    Dr. Alex Harrison Parker Postdoctoral Fellow in Planetary Astronomy Department of Astronomy University of California at Berkeley Phone: 360-599-5346 B-20 Hearst Field Annex #3411 [email protected] Berkeley, CA 94720-3411 www.astro.uvic.ca/~alexhp/ Higher Education Institution Field Degree Years University of Victoria Astronomy PhD 2007|2011. University of Washington Physics & Astronomy BSc 2005|2007. Whatcom Community College Physics AAS 2002|2005. PhD Details \Ultra-Wide Trans-Neptunian Binaries: Tracers of the Outer Solar System's History" | Advised by Dr. JJ Kavelaars, National Research Council of Canada | Thesis archived online at http://hdl.handle.net/1828/3400 | Enrolled September 2007 | Defended July 2011 | Awarded November 2011 Professional Appointments University of California at Berkeley - Postdoctoral Fellow 2013 | Present. University of California at Berkeley Department of Astronomy Ongoing support for New Horizons post-Pluto/Kuiper Belt mission development. Kuiper Belt Binaries team lead for CFHT-OSSOS Large Program. See \Ongoing Research" document. New Horizons Outer Solar System Science Fellow 2011 | 2013. Harvard-Smithsonian Center for Astrophysics, Cambridge MA USA. Survey specialist; searching for candidate Kuiper Belt Objects for NASA's New Horizons spacecraft to visit after its 2015 Pluto encounter. Perform advanced survey image analysis, trajectory analysis, target orbit and physical characterization. Manage central astrometry database and target submission to the Minor Planet Center. Science case development for remote-sensing observations of Kuiper Belt Objects at medium range (0.1-0.5 AU). National Science Foundation | Graduate Research Fellow 2008 | 2011. University of Victoria, Victoria BC Canada. PhD research in binary Kuiper Belt Object orbits, dynamics, and origin.
    [Show full text]
  • 2011 Hm102: Discovery of a High-Inclination L5 Neptune Trojan in the Search for a Post-Pluto New Horizons Target
    The Astronomical Journal, 145:96 (6pp), 2013 April doi:10.1088/0004-6256/145/4/96 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. 2011 HM102: DISCOVERY OF A HIGH-INCLINATION L5 NEPTUNE TROJAN IN THE SEARCH FOR A POST-PLUTO NEW HORIZONS TARGET Alex H. Parker1, Marc W. Buie2,DavidJ.Osip3, Stephen D. J. Gwyn4, Matthew J. Holman1, David M. Borncamp2, John R. Spencer2, Susan D. Benecchi5, Richard P. Binzel6, Francesca E. DeMeo6,Sebastian´ Fabbro4, Cesar I. Fuentes7, Pamela L. Gay8, J. J. Kavelaars4, Brian A. McLeod1, Jean-Marc Petit9, Scott S. Sheppard5, S. Alan Stern2, David J. Tholen10, David E. Trilling7, Darin A. Ragozzine1,11, Lawrence H. Wasserman12, and the Ice Hunters13 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected] 2 Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA 3 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 4 Canadian Astronomy Data Centre, National Research Council of Canada, 5071 W. Saanich Road, Victoria, BC V9E 2E7, Canada 5 Department of Terrestrial Magnetism, Carnegie Institute of Washington, 5251 Broad Branch Road NW, Washington, DC 20015, USA 6 Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 7 Department of Physics & Astronomy, Northern Arizona University, S San Francisco St, Flagstaff, AZ 86011, USA 8 The Center for Science, Technology, Engineering and Mathematics (STEM) Research, Education, and Outreach, Southern
    [Show full text]
  • SSSC Commissioning Notes
    SSSC Commissioning Notes In this document, the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Solar System Science Collaboration (SSSC) has compiled a series of commissioning notes, proposing on-sky observing strategies during commissioning that would enhance opportunities for science validation and testing of the Rubin Observatory’s data management pipelines. The SSSC has ranked the commissioning notes below into priorities (high, medium, and low) based on the expected contribution to verifying the scientific capability of Rubin Observatory and informing Year 1 LSST operations. PROPOSED HIGH PRIORITY WIDE-FAST-DEEP OBSERVING COMMISSIONING TASKS Validation of Incremental Template Generation Proposed by: Meg Schwamb & Mario Jurić ​ Email Contact for Further Information: [email protected], ​ ​ [email protected] RA(s)/Decs(s): Agnostic to the specific pointing and cadence of observations ​ Filter(s) Required: grizy ​ Brief Description of Observing strategy: ​ Wide-Fast-Deep (WFD) cadence might be preferable to fully characterize the incremental template generation pipelines, but observing strategy is flexible. The main constraint is obtaining the appropriate number of images per filter that meet the criteria for template generation. Rationale: These proposed observations will test and validate the incremental template generation capability of the data management pipelines and confirm incremental templates can be successfully generated at the start of operations for Solar System objects to be detected 1 in
    [Show full text]
  • Long-Range Kuiper Belt Targets Observed by the Hubble Space Telescope ⇑ S.D
    Icarus 246 (2015) 369–374 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus New Horizons: Long-range Kuiper Belt targets observed by the Hubble Space Telescope ⇑ S.D. Benecchi a,b, , K.S. Noll c, H.A. Weaver d, J.R. Spencer e, S.A. Stern e, M.W. Buie e, A.H. Parker f a Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719, United States b Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road, NW, Washington, DC 20015, United States c NASA Goddard Space Flight Center, 8800 Greenbelt Road, Code 693, Greenbelt, MD 20771, United States d Space Department, Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, United States e Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302, United States f Department of Astronomy, University of California at Berkeley, B-20 Hearst Field Annex #3411, Berkeley, CA 94720, United States article info abstract Article history: We report on Hubble Space Telescope (HST) observations of three Kuiper Belt Objects (KBOs), discovered Received 5 February 2014 in our dedicated ground-based search campaign, that are candidates for long-range observations from the Revised 14 April 2014 New Horizons spacecraft: 2011 JY31, 2011 HZ102, and 2013 LU35. Astrometry with HST enables both cur- Accepted 15 April 2014 rent and future critical accuracy improvements for orbit precision, required for possible New Horizons Available online 2 May 2014 observations, beyond what can be obtained from the ground. Photometric colors of all three objects are red, typical of the Cold Classical dynamical population within which they reside; they are also the Keywords: faintest KBOs to have had their colors measured.
    [Show full text]
  • 2004 KV18: a Visitor from the Scattered Disc to the Neptune Trojan Population J
    Mon. Not. R. Astron. Soc. 426, 159–166 (2012) doi:10.1111/j.1365-2966.2012.21717.x 2004 KV18: a visitor from the scattered disc to the Neptune Trojan population J. Horner1 and P. S. Lykawka2 1Department of Astrophysics, School of Physics, University of New South Wales, Sydney, NSW 2052, Australia 2Astronomy Group, Faculty of Social and Natural Sciences, Kinki University, Shinkamikosaka 228-3, Higashiosaka-shi, Osaka 577-0813, Japan Accepted 2012 July 12. Received 2012 July 12; in original form 2012 June 14 ABSTRACT Downloaded from We have performed a detailed dynamical study of the recently identified Neptunian Trojan 2004 KV18, only the second object to be discovered librating around Neptune’s trailing Lagrange point, L5. We find that 2004 KV18 is moving on a highly unstable orbit, and was most likely captured from the Centaur population at some point in the last ∼1 Myr, having originated in http://mnras.oxfordjournals.org/ the scattered disc, beyond the orbit of Neptune. The instability of 2004 KV18 is so great that many of the test particles studied leave the Neptunian Trojan cloud within just ∼0.1–0.3 Myr, and it takes just 37 Myr for half of the 91 125 test particles created to study its dynamical behaviour to be removed from the Solar system entirely. Unlike the other Neptunian Trojans previously found to display dynamical instability on 100-Myr time-scales (2001 QR322 and 2008 LC18), 2004 KV18 displays such extreme instability that it must be a temporarily captured Trojan, rather than a primordial member of the Neptunian Trojan population.
    [Show full text]
  • Institute for Astronomy University of Hawai'i at M¯Anoa Publications in Calendar Year 2013
    Institute for Astronomy University of Hawai‘i at Manoa¯ Publications in Calendar Year 2013 Aberasturi, M., Burgasser, A. J., Mora, A., Reid, I. N., Barnes, J. E., & Privon, G. C. Experiments with IDEN- Looper, D., Solano, E., & Mart´ın, E. L. Hubble Space TIKIT. In ASP Conf. Ser. 477: Galaxy Mergers in an Telescope WFC3 Observations of L and T dwarfs. Evolving Universe, 89–96 (2013) Mem. Soc. Astron. Italiana, 84, 939 (2013) Batalha, N. M., et al., including Howard, A. W. Planetary Albrecht, S., Winn, J. N., Marcy, G. W., Howard, A. W., Candidates Observed by Kepler. III. Analysis of the First Isaacson, H., & Johnson, J. A. Low Stellar Obliquities in 16 Months of Data. ApJS, 204, 24 (2013) Compact Multiplanet Systems. ApJ, 771, 11 (2013) Bauer, J. M., et al., including Meech, K. J. Centaurs and Scat- Al-Haddad, N., et al., including Roussev, I. I. Magnetic Field tered Disk Objects in the Thermal Infrared: Analysis of Configuration Models and Reconstruction Methods for WISE/NEOWISE Observations. ApJ, 773, 22 (2013) Interplanetary Coronal Mass Ejections. Sol. Phys., 284, Baugh, P., King, J. R., Deliyannis, C. P., & Boesgaard, A. M. 129–149 (2013) A Spectroscopic Analysis of the Eclipsing Short-Period Aller, K. M., Kraus, A. L., & Liu, M. C. A Pan-STARRS + Binary V505 Persei and the Origin of the Lithium Dip. UKIDSS Search for Young, Wide Planetary-Mass Com- PASP, 125, 753–758 (2013) panions in Upper Sco. Mem. Soc. Astron. Italiana, 84, Beaumont, C. N., Offner, S. S. R., Shetty, R., Glover, 1038–1040 (2013) S. C.
    [Show full text]
  • A Proposal for a Research Settlement on 2011 HM102 and a Framework
    Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 7 April 2021 doi:10.20944/preprints202104.0215.v1 1 The Trojan Initiative: A Proposal For A Research Settlement On 2011 HM102 and A Framework for Future Settlement on Asteroids Briana Chen1*, Geetika Chitturi1*, Archit Kalra1*, Raghav Sriram1* 1: Carmel High School *: All authors contributed equally to the production of this manuscript and are hence written in alphabetical order. © 2021 by the author(s). Distributed under a Creative Commons CC BY license. Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 7 April 2021 doi:10.20944/preprints202104.0215.v1 2 Contents Abstract…………...………………………………………………………………………….....…4 Reason for Settling 2011 HM102…………………………………………………………....……...5 Population……..……………………………………………………………………………….….6 Travel to Settlement..……………………………………………………………………………...7 Antimatter Engine…………………………………………………………………………7 Settlement Materials .……………………………………………………………………………..9 Settlement Design .………………………………………………………………………………11 A Model For the Simulation of Artificial Gravity…………………………………….....11 Layout of Structure……………………………………………………………………....13 Power Sources…………………………………………………………………………...16 Shielding and Protection………………………………………………………….……..18 Maintenance of Life.………………………………………………………………………….....20 Importance of Growing Food………………………………………………….……...…20 Sustainable Crop Growth…………………………………………………….……...…..20 Water Recovery…………………………………………………………….……...…….22 Oxygen Recycling………………………………………………………….……………23 Eliminating Carbon Dioxide…………………………………………………………….24 Air Filtration………………………………………………….………………….………24
    [Show full text]
  • The Dynamics of Ringed Small Bodies
    THE DYNAMICS OF RINGED SMALL BODIES A Thesis Submitted by Jeremy R. Wood For the Award of Doctor of Philosophy 2018 Abstract In 2013, the startling discovery of a pair of rings around the Centaur 10199 Chariklo opened up a new subfield of astronomy - the study of ringed small bodies. Since that discovery, a ring has been discovered around the dwarf planet 136108 Haumea, and a re-examination of star occultation data for the Centaur 2060 Chiron showed it could have a ring structure of its own. The reason why the discovery of rings around Chariklo or Chiron is rather shocking is because Centaurs frequently suffer close encounters with the giant planets in the Centaur region, and these close encounters can not only fatally destroy any rings around a Centaur but can also destroy the small body itself. In this research, we determine the likelihood that any rings around Chariklo or Chiron could have formed before the body entered the Centaur region and survived up to the present day by avoiding ring-destroying close encounters with the giant planets. And in accordance with that, develop and then improve a scale to measure the severity of a close encounter between a ringed small body and a planet. We determine the severity of a close encounter by finding the minimum dis- tance obtained between the small body and the planet during the encounter, dmin, and comparing it to the critical distances of the Roche limit, tidal dis- ruption distance, the Hill radius and \ring limit". The values of these critical distances comprise our close encounter severity scale.
    [Show full text]
  • The Proposed Origin of Our Solar System with Planet Migration DOI
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Digital Commons The Proceedings of the International Conference on Creationism Volume 8 Article 35 2018 The proposed origin of our solar system with planet migration DOI: https://doi.org/10.15385/jpicc.2018.8.1.10 Wayne R. Spencer none Follow this and additional works at: http://digitalcommons.cedarville.edu/icc_proceedings Part of the The unS and the Solar System Commons Browse the contents of this volume of The Proceedings of the International Conference on Creationism. Recommended Citation Spencer, W.R. 2018. The proposed origin of our solar system with planet migration. In Proceedings of the Eighth International Conference on Creationism, ed. J.H. Whitmore, pp. 71–81. Pittsburgh, Pennsylvania: Creation Science Fellowship. Spencer, W.R. 2018. The proposed origin of our solar system with planet migration. In Proceedings of the Eighth International Conference on Creationism, ed. J.H. Whitmore, pp. 71–81. Pittsburgh, Pennsylvania: Creation Science Fellowship. THE PROPOSED ORIGIN OF OUR SOLAR SYSTEM WITH PLANET MIGRATION Wayne R. Spencer, Independent scholar, Irving, TX 75063 USA, [email protected] ABSTRACT Two new models to explain the origin and history of our solar system are reviewed from a creation perspective, the Grand Tack model and the Nice model. These new theories propose that the four outer planets formed closer to the Sun, as well as closer together, than today. Then their orbits underwent periods of migration. Theories developed in the research on extrasolar planet systems are today being applied to our own solar system.
    [Show full text]