DOCSLIB.ORG

Orbit Globe Equatorial Axis Planet Sidereal Perihelion Aphelion

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Orbit Globe Equatorial Axis Planet Sidereal Perihelion Aphelion Table 1 Planets Orbit I Globe Equatorial Axis Planet Sidereal Perihelion Aphelion lnclinationl Diameter Oblateness Mass Density Albedo Tilt Period* Satellites Period (AU) (AU) (deg) . (km) (Earth=l)(water=J) (deg) (d h m) Mercury 87.97 d 0.31 0.47 7_.0 4878 0.0 0.06 5.4 0.06 0 58 15 30.2 0 Venus 224.70d 0.72 0.73 .3.4 12104 0.0 0.82 5.2 0.72 177 243 0 R 0 Earth 365.26d 0.98 1.02 0.0 12 756 0.0034 1.00 5.5 0.39 23.4 23 56.1 1 Mars 686.98d 1.38 1.67 1.8 6787 0.005 0.11 3.9 0.16 25.0 1 0 37.4 2 Jupiter 11.86 y 4.95 5.45 1.3 142800 0.065 317.83 1.3 0.70 3.1 9 50.5 16 & rings Saturn 29.46y 9.01 10.07 2.5 120000 0.108 95.17 0.7 0.75 26.7 10 14 +22& rings Uranus 84.01 y 18.28 20.09 0.8 50800 0.030 14.50 1.3 0.90 97.9 -16 R 5 & rings Neptune 164.79y 29.80 30.32 1.8 48600 0.026 17.20 1.8 0.82 29.6 -18 2 Pluto 247.7y 29.6 49.3 17.2 3000? 0 0.002 1.1? 0.9? 118? 6 9 17 1 *R indicates retrograde axial rotation. The rotation periods for Jupiter and Saturn refer to equatorial regions; the periods exceed 9h 5 5m and 1Oh 38m at higher latitudes, respectively. ,. ~ 427 Table2 P11111etary Satellites PLANET li!ar Diameter Orbital Eccentricity Orbital Inclination & of (km) Radius Period (") Satellite Discovery (Ift km) (days) EARTH moon 3476 384.4 0.055 27.32 23.4 MARS Phobos 1877 27 X 22 X 19 9.38 0.015 0.32 1.0 Deimos 1877 15 X 12 X 11 23.46 0.001 1.26 1.8 JUPITER Metis 1979 40 128 0.29 Adrastea 1979 24x20x16 129 0.30 Amalthea 1892 270 X 170 X 150 181 0.003 0.50 0.5 Thebe 1979 100 222 0.013 0.67 0.9 Io 1610 3630 422 0.004 1.77 0.0 Europa 1610 3050 671 0.009 3.55 0.5 Ganymede 1610 5260 1070 0.002 7.15 0.2 Callisto 1610 4800 1883 0.007 16.69 0.5 Leda 1974 20 11094 0.148 239 26 Himalia 1904 180 11480 0.158 250.6 28 Lysithea 1938 40 11720 0.107 259.2 29 Elara 1905 80 11740 0.207 259.7 25 Ananke 1951 30 21200 0.17 631 R 147 Car me 1938 40 22600 0.21 692R 164 Pasiphae 1908 50 23500 0.38 735 R 145 Sin ope 1914 40 23700 0.28 758R 153 SATURN 1980 S28 1980 40 X 20 138 0.61 0 1980 S27 1980 100 139 0.61 0 1980 S26 1980 100 142 0.63 0 1980 S3 1978 90 X 40 151 0.69 0 1980 S1 1978 100 151 0.69 0 Mimasc-o 1982 10 186 0.94 1.5 Mimas 1789 390 186 0.020 0.94 1.5 Enceladus 1789 500 238 0.004 1.37 0.0 Tethys 1684 1050 295 0.000 1.89 1.1 1980S25 1980 35 295 1.9 1980 S13 1980 35 295 1.9 Tethys c-o 1982 15 295 1.9 0 1982 15 350 2.4 Dione 1684 1120 377 0.002 2.74 0.0 1980 S6 1980 160 378 2.7 Dione c-o 1982 15 378 0.3 1982 470 Rhea 1672 1530 527 0.001 4.52 0.3 Titan 1655 5150 1222 0.029 15.95 0.3 Hyperion 1848 400 X 250 X 240 1481 0.104 21.28 0.4 Iapetus 1671 1440 3560 0.028 79.33 14.7 Phoebe 1898 160 12950 0.163 550.34R 150 428 Table 2 Planetary Satellites PLANET ~ar Diameter Orbital Eccentricity Orbital Inclination & of (km) Radius Period (") Satellite Discovery (HI km) (days) URANUS Miranda 1948 400 130 0.027 1.41 4 Ariel 1851 1300 191 0.003 2.52 0.3 Umbriel 1851 1100 266 0.004 4.14 0.4 Titania 1787 1600 436 0.002 8.71 0.1 Oberon 1787 1600 583 0.001 13.46 0.1 NEPTUNE Triton 1846 3800 355 0.000 5.88R 160 Nereid 1949 300 5510 0.75 360.2 28 PLUTO Charon 1978 1000? 20 0? 6.39 0? Note: The diameters given for the smaller satellites of Jupiter, and for many of the satellites of Saturn, Uranus, Neptune, and Pluto, are uncertain. The orbits of the outer satellites of Jupiter vary considerably with time. The distances refer to the centre of the parent planet and the inclinations to the plane of the equator of the planet. R indicates retrograde motion. c-o in a satellite name indicates co-orbital. 429 Table 3 Minor planets No. Name Discovery Period Perihelion Aphelion Inc Diameter Rotation Year (years) (AU) (AU) (0) (km) (hours) I Ceres 1801 4.60 2.55 2.98 10.6 1003 9.1 2 Pallas 1802 4.61 2.11 3.42 34.8 540 10.5 3 Juno 1804 4.36 1.98 3.35 13.0 247 7.2 4 Vesta 1807 3.63 2.15 2.57 7.1 5\55 10.7 5 Astraea 1845 4.14 2.10 3.06 5.3 117 16.8 6 Hebe 1847 3.78 1.93 2.92 14.8 201 7.3 7 Iris 1847 3.69 1.84 2.94 5.5 209 7.1 10 Hygiea 1849 5.59 2.84 3.46 3.8 450 18.0 15 Eunomia 1851 4.30 2.14 3.14 11.7 272 6.1 31 Euphrosyne 1854 5.61 2.45 3.86 26.3 370 ? 433 Eros 1898 1.76 1.13 1.78 10.8 23 5.3 588 Achilles 1906 11.90 4.44 5.98 10.3 50 ? 944 Hidalgo 1920 14.04 2.00 9.64 42.5 15 ? 1221 Amor 1932 2.66 1.08 2.76 11.9 0.5 ? 1566 Icarus 1949 1.12 0.19 1.97 23.0 I 2.3 1862 Apollo 1932 1.78 0.65 2.29 6.3 I ? 2060 Chiron 1977 50.68 8.51 18.88 6.9 300? ?- 2062 A ten 1976 0.95 0.79 1.14 18.9 I ? - Adonis 1936 2.56 0.44 3.30 1.4 0.3 ? - Hermes 1937 2.10 0.62 2.66 6.2 0.5 ? Table 4 Meteor Showers Shower Normal Limits ZHRatMax. Quadrantids Jan.l-6 110 Corona Australids Mar.l4-18 5 April Lyrids Apr.l9-24 12 ., -Aquarids Mayl-8 20 JuneLyrids June 10--21 8 Ophiuchids Junel7-26 6 Capricornids July 10--Aug. 15 6 8 -Aquarids July 15-Aug.l5 35 Pisces Australids July 15-Aug. 20 8 a -Capricornids July 15-Aug. 25 8 Perseids July 25-Aug. 18 68 Cygnids Aug.l9-22 4 Orionids Oct.l6-26 30 Taurids Oct. 20--Nov. 30 12 Cepheids Nov. 7-11 8 Leonids Nov.l5-19 10 Phoenicids Dec.4-5 5 Geminids Dec. 7-15 58 Ursids Dec.l7-24 5 430 Table S Constellations Andromeda And Delphinus Del Perseus Per Antlia Ant Dorado Dor Phoenix Phe Apus Aps Draco Ora Pictor Pic Aquarius Aqr Equuleus Equ Pisces Psc Aquila Aql Eridanus Eri Piscis Austrinus PsA Ara Ara Fomax For Puppis Pup Aries Ari Gemini Gem Pyxis Pyx Auriga Aur Grus Gru Reticulum Ret Bootes Boo Hercules Her Sagitta Sge Caelum Cae Horologium Hor Sagittarius Sgr Camelopardalis Cam Hydra ,Hya Scorpius Sco Cancer Cnc Hydrus Hyi Sculptor Sci Canes Venatici CVn Indus Ind Scutum Set Canis Major CMa Lacerta Lac Serpens Ser Canis Minor CMi Leo Leo Sextans Sex Capricomus Cap Leo Minor LMi Taurus Tau Carina Car Lepus Lep Telescopium Tel Cassiopeia Cas Libra Lib Triangulum Tri Centaurus Cen Lupus Lup Triangulum Australe TrA Cepheus Cep Lynx Lyn Tucana Tuc Cetus Cet Lyra Lyr Ursa Major UMa Chameleon Cha Mensa Men Ursa Minor UMi Circinus Cir Microscopium Mic Vela Vel Columba Col Monoceros Mon Virgo Vir Coma Berenices Com Musca Mus Volans Vol Corona Australis CrA Norma Nor Vulpecula Vul Corona Borealis CrB Octans Oct Corvus Crv Ophiuchus Oph Crater Crt Orion Ori Crux Cru Pavo Pav Cygnus Cyg Pegasus Peg 431 Table 6 The Twenty-Five Brightest Stars Star Position (197 5) Apparent Distance Spectral Absolute magnitude (parsecs) Type Magnitude a 8 (m.J (M) Sirius, a CMa (/1 44.<F -16°41' -1.5* 2.7 A1V +1.4 Canopus, a Car 6 23.6 -52 41 -0.7 60 FOil -4.6 a Centauri 14 38.0 -60 44 -0.3* 1.31 G2V +4.2 Arcturus, a Boo 14 14.5 +19 19 -0.1 11 K2III -0.3 Vega, aLyr 18 36.0 +38 46 0.0 8.1 AOV +0.5 Capella, a.Aur 5 14.8 +45 52 0.1* 14 08III -0.6 Rigel, pOri 5 13.3 -8 14 0.1* 250 B8Ia -7.1 Procyon, a CMi 7 38.0 +5 17 0.4* 3.5 F5 IV-V +2.7 Achemar, a Eri 1 37.8 -57 22 0.5 35 B5V -2.2 pCentauri 14 02.1 -60 15 0.6* 120 B1 III -4.8 Altair, aAql 19 49.5 +8 48 0.8 5.1 A7IV-V +2.3 Betelgeuse, a Ori 5 53.8 +7 24 o.8t 200 M2Iab -5.7 Aldebaran, a Tau 4 34.0 +16 28 o.8* 21 K5 III -0.8 a Crucis 12 25.2 -63 00 0.9* 80 BliV -3.7 Spica, aVir 13 23.9 -11 01 LOt 65 B1V -3.1 Antares, aSco 16 27.8 -26 22 l.O*t 130 M1Ib -4.7 Pollux, p Gem 7 43.8 +28 05 1.2 11 KOIII +1.0 Fomalhaut, aPsA 22 56.2 -29 45 1.2 7 A3V +1.9 Deneb, aCyg 20 40.6 +45 11 1.3 430 A2Ia -7.2 pcrucis 12 46.2 -59 33 1.3 130 BO IIII -4.3 Regulus, aLeo 10 7.0 +12 5 t.J• 26 B7V -0.8 Adhara, £ CMa 6 57.7 -28 56 1.5 200 B211 -5.0 Castor, aGem 7 33.0 +31 56 1.6 14 A1V +0.8 Shaula, ASco 17 31.8 -37 5 1.6 96 B2IV -3.3 Bellatrix, Y Ori 5 23.8 +6 20 1.6 140 B2III -4.1 *Multiple star: Illy is integrated magnitude tVariable star 432 Table 7 Nearest Stan Star Position (1975) Distance Prop.Mot.App.mag.
Load more

Recommended publications
  • Asteroid Shape and Spin Statistics from Convex Models J
    Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen To cite this version: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen. Asteroid shape and spin statistics from convex models. Icarus, Elsevier, 2008, 198 (1), pp.91. 10.1016/j.icarus.2008.07.014. hal-00499092 HAL Id: hal-00499092 https://hal.archives-ouvertes.fr/hal-00499092 Submitted on 9 Jul 2010 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. Accepted Manuscript Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen PII: S0019-1035(08)00283-2 DOI: 10.1016/j.icarus.2008.07.014 Reference: YICAR 8734 To appear in: Icarus Received date: 18 September 2007 Revised date: 3 July 2008 Accepted date: 7 July 2008 Please cite this article as: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen, Asteroid shape and spin statistics from convex models, Icarus (2008), doi: 10.1016/j.icarus.2008.07.014 This is a PDF file of an unedited manuscript that has been accepted for publication.
    [Show full text]
  • Occultation Newsletter Volume 8, Number 4
    Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date.
    [Show full text]
  • Zákryt Jasné Hvězdy Saturnem
    Zákrytová a astrometrická sekce ČAS leden 2006 (1) Zajímavosti: NENECHTE SI UJÍT Zákryt jasné hv ězdy Saturnem 25. ledna 2006 ve čer mimo jiné i Evropu čeká velice zajímavá ř ě Č podívaná. Planeta Saturn okrášlená prstencem p řejde p řes relativn ě Situace, jak vypadá p i pohledu z hv zdy. asy udávané v malé vložené ě ě č jasnou hv ězdu a ze Zem ě budeme mít možnost sledovat nejen zákryt tabulce jsou platné pro Mainz (N mecko). Pro jiná místa v Evrop jsou asy v tabulce za článkem. stálice vlastní planetou, ale i její poblikávání za jednotlivými prstenci. Velice zajímavé bude jist ě pokusit se celý úkaz nahrát speciálními videokamerami v ohnisku dlouhofokálních teleobjektiv ů či dalekohled ů. Zajímavá a nevšední podívaná však čeká jist ě i na ty, kdo se na úkaz budou chtít pouze vizuáln ě podívat. Lednový zákryt hv ězdy Saturnem je jist ě zajímavou údálostí, ale nemá p říliš velkou publicitu. Úkaz bude viditelný z Evropy, Afriky a Asie. P řičemž z jižní Afriky bude možno sledovat pouze zákryty hv ězdy prstenci a zákryt vlastní planetou tuto oblast již mine. U nás, ve st řední Evrop ě, by úkaz m ěl za čít v 18:45 UT, kdy se hv ězda dostane k vn ějšímu okraji soustavy prstenc ů. V tom čase bude planeta již dostate čně vysoko nad východním obzorem (h=26°; A=92°). Zákryt Pr ůchod hv ězdy oblastí systému satelit ů planety Saturn p ři pohledu ze Země kotou čkem planety pak nastane v intervalu 20:08 UT (D – vstup) až 20:49 (R – (geocentrický pohled).
    [Show full text]
  • Occultations by Major and Minor Planets – 2008 Region 8
    Occultations by major and minor planets ± 2008 Region 8 2008 jan 1 19h48.8m A08_01079 2008 jan 3 10h36.1m A08_01012 2008 jan 4 12h48.4m A08_01064 2008 jan 9 12h 7.2m B08_01003 976 Benjamina UCAC2 26000295 76 Freia TYC 1320−00481−1 678 Fredegundis UCAC2 38786034 2003TK58 UCAC2 39974889 Diam = 86.6 m = 11.5 Diam = 190.0 m = 11.8 Diam = 44.0 m = 11.1 Diam = 109.6 m = 14.0 m = 14.9 m = 12.0 m = 11.8 m = 24.1 Dur = 3.4s Dmag = 3.4 Dur = 17.8s Dmag = 0.8 Dur = 4.4s Dmag = 1.1 Dur = 5.1s Dmag = 10.1 Sun: 74° Moon: 2° Sun: 167° Moon: 136° Sun: 169° Moon: 125° Sun: 148° Moon: 136° 2008 jan 11 17h 0.4m A08_01067 2008 jan 14 14h44.1m B08_01002 2008 jan 15 12h 0.7m A08_01029 2008 jan 15 14h58.1m A08_01046 694 Ekard TYC 6114−00532−1 2000YX1 UCAC2 39092566 227 Philosophia TYC 2424−00058−1 478 Tergeste UCAC2 31677375 Diam = 92.7 m = 12.4 Diam = 138.0 m = 13.4 Diam = 90.1 m = 9.8 Diam = 82.0 m = 11.6 m = 15.3 m = 23.3 m = 13.9 m = 12.1 Dur = 7.3s Dmag = 3.0 Dur = 9.3s Dmag =10.0 Dur = 6.4s Dmag = 4.2 Dur = 7.3s Dmag = 1.0 Sun: 91° Moon: 129° Sun: 130° Moon: 56° Sun: 157° Moon: 73° Sun: 156° Moon: 108° 2008 jan 20 14h27.5m A08_01015 2008 jan 23 12h60.0m A08_01042 2008 jan 24 8h 2.9m A08_01085 2008 jan 26 12h33.3m A08_01086 82 Alkmene HIP 59771 424 Gratia TYC 1950−00948−1 47171 1999TC36 TYC 4681−01120−1 2001XU254 TYC 1373−02131−1 Diam = 63.6 m = 9.7 Diam = 90.5 m = 11.4 Diam = 346.7 m = 11.5 Diam = 182.0 m = 10.8 m = 12.0 m = 13.2 m = 20.0 m = 22.6 Dur = 10.5s Dmag = 2.4 Dur = 7.9s Dmag = 2.0 Dur = 20.7s Dmag = 8.5 Dur = 7.3s Dmag = 11.8 Sun: 116° Moon:
    [Show full text]
  • Appendix 1 1311 Discoverers in Alphabetical Order
    Appendix 1 1311 Discoverers in Alphabetical Order Abe, H. 28 (8) 1993-1999 Bernstein, G. 1 1998 Abe, M. 1 (1) 1994 Bettelheim, E. 1 (1) 2000 Abraham, M. 3 (3) 1999 Bickel, W. 443 1995-2010 Aikman, G. C. L. 4 1994-1998 Biggs, J. 1 2001 Akiyama, M. 16 (10) 1989-1999 Bigourdan, G. 1 1894 Albitskij, V. A. 10 1923-1925 Billings, G. W. 6 1999 Aldering, G. 4 1982 Binzel, R. P. 3 1987-1990 Alikoski, H. 13 1938-1953 Birkle, K. 8 (8) 1989-1993 Allen, E. J. 1 2004 Birtwhistle, P. 56 2003-2009 Allen, L. 2 2004 Blasco, M. 5 (1) 1996-2000 Alu, J. 24 (13) 1987-1993 Block, A. 1 2000 Amburgey, L. L. 2 1997-2000 Boattini, A. 237 (224) 1977-2006 Andrews, A. D. 1 1965 Boehnhardt, H. 1 (1) 1993 Antal, M. 17 1971-1988 Boeker, A. 1 (1) 2002 Antolini, P. 4 (3) 1994-1996 Boeuf, M. 12 1998-2000 Antonini, P. 35 1997-1999 Boffin, H. M. J. 10 (2) 1999-2001 Aoki, M. 2 1996-1997 Bohrmann, A. 9 1936-1938 Apitzsch, R. 43 2004-2009 Boles, T. 1 2002 Arai, M. 45 (45) 1988-1991 Bonomi, R. 1 (1) 1995 Araki, H. 2 (2) 1994 Borgman, D. 1 (1) 2004 Arend, S. 51 1929-1961 B¨orngen, F. 535 (231) 1961-1995 Armstrong, C. 1 (1) 1997 Borrelly, A. 19 1866-1894 Armstrong, M. 2 (1) 1997-1998 Bourban, G. 1 (1) 2005 Asami, A. 7 1997-1999 Bourgeois, P. 1 1929 Asher, D.
    [Show full text]
  • Infrared Spectroscopy of Large, Low-Albedo Asteroids: Are Ceres and Themis Archetypes Or Outliers?
    Infrared Spectroscopy of Large, Low-Albedo Asteroids: Are Ceres and Themis Archetypes or Outliers? Andrew S. Rivkin1, Ellen S. Howell2, Joshua P. Emery3 1. Johns Hopkins University Applied Physics Laboratory 2. University of Arizona 3. University of Tennessee Corresponding author: Andrew Rivkin ([email protected]) Key points: • The largest low-albedo asteroids appear to be unrepresented in the meteorite collection • Reflectance spectra in the 3-µm spectral region, and presumably compositions, similar to Ceres and Themis appear to be common in low-albedo asteroids > 200 km diameter • The asteroid 324 Bamberga appears to have hemispherical-scale variation in its reflectance spectrum, and in places has a spectrum reminiscent of Comet 67P. Submitted to Journal of Geophysical Research 17 September 2018 Revised 27 February 2019 Accepted 12 April 2019 1 Abstract: Low-albedo, hydrated objects dominate the list of the largest asteroids. These objects have varied spectral shapes in the 3-µm region, where diagnostic absorptions due to volatile species are found. Dawn’s visit to Ceres has extended the view shaped by ground-based observing, and shown that world to be a complex one, potentially still experiencing geological activity. We present 33 observations from 2.2-4.0 µm of eight large (D > 200 km) asteroids from the C spectral complex, with spectra inconsistent with the hydrated minerals we see in meteorites. We characterize their absorption band characteristics via polynomial and Gaussian fits to test their spectral similarity to Ceres, the asteroid 24 Themis (thought to be covered in ice frost), and the asteroid 51 Nemausa (spectrally similar to the CM meteorites).
    [Show full text]
  • The Euphrosyne Family's Contribution to the Low Albedo Near-Earth
    The Euphrosyne family's contribution to the low albedo near-Earth asteroids Joseph R. Masiero1, V. Carruba2, A. Mainzer1, J. M. Bauer1, C. Nugent3 ABSTRACT The Euphrosyne asteroid family is uniquely situated at high inclination in the outer Main Belt, bisected by the ν6 secular resonance. This large, low albedo family may thus be an important contributor to specific subpopulations of the near-Earth objects. We present simulations of the orbital evolution of Euphrosyne family members from the time of breakup to the present day, focusing on those members that move into near- Earth orbits. We find that family members typically evolve into a specific region of orbital element-space, with semimajor axes near ∼ 3 AU, high inclinations, very large eccentricities, and Tisserand parameters similar to Jupiter family comets. Filtering all known NEOs with our derived orbital element limits, we find that the population of candidate objects is significantly lower in albedo than the overall NEO population, although many of our candidates are also darker than the Euphrosyne family, and may have properties more similar to comet nuclei. Followup characterization of these candidates will enable us to compare them to known family properties, and confirm which ones originated with the breakup of (31) Euphrosyne. 1. Introduction The Euphrosyne asteroid family occupies a unique place in orbital element space among fam- ilies, located in the outer Main Belt at very high inclination, as shown in Figure 1. It is also the only asteroid family that is bisected by the ν6 secular orbital resonance. The inner-most portion of this resonance (semimajor axis< 2:5 AU) has been shown to be a primary mechanism for moving asteroids onto near-Earth orbits with relatively long lifetimes (Bottke et al.
    [Show full text]
  • The Planetary and Lunar Ephemeris DE 421
    IPN Progress Report 42-178 • August 15, 2009 The Planetary and Lunar Ephemeris DE 421 William M. Folkner,* James G. Williams,† and Dale H. Boggs† The planetary and lunar ephemeris DE 421 represents updated estimates of the orbits of the Moon and planets. The lunar orbit is known to submeter accuracy through fitting lunar laser ranging data. The orbits of Venus, Earth, and Mars are known to subkilometer accu- racy. Because of perturbations of the orbit of Mars by asteroids, frequent updates are needed to maintain the current accuracy into the future decade. Mercury’s orbit is determined to an accuracy of several kilometers by radar ranging. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of spacecraft tracking and modern ground-based astrometry. The orbits of Uranus, Neptune, and Pluto are not as well deter- mined. Reprocessing of historical observations is expected to lead to improvements in their orbits in the next several years. I. Introduction The planetary and lunar ephemeris DE 421 is a significant advance over earlier ephemeri- des. Compared with DE 418, released in July 2007,1 the DE 421 ephemeris includes addi- tional data, especially range and very long baseline interferometry (VLBI) measurements of Mars spacecraft; range measurements to the European Space Agency’s Venus Express space- craft; and use of current best estimates of planetary masses in the integration process. The lunar orbit is more robust due to an expanded set of lunar geophysical solution parameters, seven additional months of laser ranging data, and complete convergence.
    [Show full text]
  • Organic Matter and Associated Minerals on the Dwarf Planet Ceres
    minerals Review Organic Matter and Associated Minerals on the Dwarf Planet Ceres Maria Cristina De Sanctis 1,* and Eleonora Ammannito 2 1 Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy 2 Agenzia Spaziale Italiana, Via del Politecnico, 00133 Roma, Italy; [email protected] * Correspondence: [email protected] Abstract: Ceres is the largest object in the main belt and it is also the most water-rich body in the inner solar system besides the Earth. The discoveries made by the Dawn Mission revealed that the composition of Ceres includes organic material, with a component of carbon globally present and also a high quantity of localized aliphatic organics in specific areas. The inferred mineralogy of Ceres indicates the long-term activity of a large body of liquid water that produced the alteration minerals discovered on its surface, including ammonia-bearing minerals. To explain the presence of ammonium in the phyllosilicates, Ceres must have accreted organic matter, ammonia, water and carbon present in the protoplanetary formation region. It is conceivable that Ceres may have also processed and transformed its own original organic matter that could have been modified by the pervasive hydrothermal alteration. The coexistence of phyllosilicates, magnetite, carbonates, salts, organics and a high carbon content point to rock–water alteration playing an important role in promoting widespread carbon occurrence. Keywords: Ceres; asteroids; organics; aliphatics; solar system Citation: De Sanctis, M.C.; Ammannito, E. Organic Matter and Associated Minerals on the Dwarf 1. Ceres: A Dwarf Planet in the Main Belt Planet Ceres. Minerals 2021, 11, 799.
    [Show full text]
  • Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites
    University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2013 Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites Driss Takir [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Part of the The Sun and the Solar System Commons Recommended Citation Takir, Driss, "Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites. " PhD diss., University of Tennessee, 2013. https://trace.tennessee.edu/utk_graddiss/1783 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Driss Takir entitled "Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Harry Y. McSween Jr., Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffery E. Moersch, Michael W. Guidry Accepted for the Council: Carolyn R. Hodges Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Driss Takir May 2013 Copyright © 2013 by Driss Takir All rights reserved.
    [Show full text]
  • Cumulative Index to Volumes 1-45
    The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) ..................
    [Show full text]
  • TRAPPIST Asteroid Lightcurves
    http://lib.uliege.ac.be http://matheo.uliege.be TRAPPIST asteroid lightcurves Auteur : Ferrais, Marin Promoteur(s) : Jehin, Emmanuel Faculté : Faculté des Sciences Diplôme : Master en sciences spatiales, à finalité approfondie Année académique : 2017-2018 URI/URL : www.trappist.ulg.ac.be; http://hdl.handle.net/2268.2/5023 Avertissement à l'attention des usagers : Tous les documents placés en accès ouvert sur le site le site MatheO sont protégés par le droit d'auteur. Conformément aux principes énoncés par la "Budapest Open Access Initiative"(BOAI, 2002), l'utilisateur du site peut lire, télécharger, copier, transmettre, imprimer, chercher ou faire un lien vers le texte intégral de ces documents, les disséquer pour les indexer, s'en servir de données pour un logiciel, ou s'en servir à toute autre fin légale (ou prévue par la réglementation relative au droit d'auteur). Toute utilisation du document à des fins commerciales est strictement interdite. Par ailleurs, l'utilisateur s'engage à respecter les droits moraux de l'auteur, principalement le droit à l'intégrité de l'oeuvre et le droit de paternité et ce dans toute utilisation que l'utilisateur entreprend. Ainsi, à titre d'exemple, lorsqu'il reproduira un document par extrait ou dans son intégralité, l'utilisateur citera de manière complète les sources telles que mentionnées ci-dessus. Toute utilisation non explicitement autorisée ci-avant (telle que par exemple, la modification du document ou son résumé) nécessite l'autorisation préalable et expresse des auteurs ou de leurs ayants droit. UNIVERSITY OF LIÈGE FACULTY OF SCIENCES DEPARTMENT OF ASTROPHYSICS,GEOPHYSICS AND OCEANOGRAPHY MASTER THESIS TRAPPIST ASTEROID LIGHTCURVES Composite lightcurve of (20) Massalia A thesis presented for the degree of Master in Space Sciences by MARIN FERRAIS Under the supervision of Emmanuël Jehin Academic Year 2017 − 2018 Contents Contents 2 1 Introduction 5 2 About asteroids 7 2.1 Introduction...........................................
    [Show full text]