DOCSLIB.ORG

Star Empire Map Outline

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Gl 25 GJ 1029 1.3 Gl 26 Gl 25 B Gl 60 Gl 32 1.3 1.0 Nu Phoenicis 2.0 Gl 32 B Gl 40 Gl 60 B GJ 2010 1.4 1.6 1.9 1.2 1.4 Gl 40 B GJ 1033 Gl 60 C 2.1 2.2 2.1 2.1 2.5 3.6 NN 3061 B 2.0 4.0 2.2 1.1 0.9 NN 3060 NN 3085 0.7 Gl 57 GJ 2019 NN 3088 1.8 2.3 1.2 GJ 2021 GJ 1036 3.1 Gl 42 3.5 NN 3092 B NN 3107 1.3 1.8 3.8 Gl 16 5.7 54 Piscium GJ 1028 2.5 1.9 GJ 1050 4.2 GJ 1031 NN 3079 1 Tau 1 Eridani NN 3198 0.6 2.2 2.2 3.0 4.3 NN 3052 1.8 1.3 2.2 1.1 NN 3039 1.5 2.1 2.7 2.5 2.4 1.8 1.2 2.3 1.5 1.2 1.9 NN 3070 2.0 1.8 NN 3148 1.1 NN 3096 2.0 NN 3111 Epsilon Sulptoris 0.6 Alpha Fornacis 1.5 NN 3162 Gl 18 2.1 2.9 GJ 1007 Gl 127 B GJ 1046 3.8 2.2 GJ 2020 0.9 GJ 1014 Gl 64 2.4 GJ 2012 1.9 NN 3119 1.5 NN 3010 1.3 1.3 Star Empire Map Outline 3.0 2.4 Hip 5663 4.7 Hip 7576 2.8 1.9 Gl 79 3.5 Gl 46 2.1 1.7 6.5 3.6 4.5 5.6 3.7 0.4 GJ 1024 1.9 2.1 2.1 2.0 NN 3051 GJ 1041 B 1.7 NN 3140 Gl 101.1 Gl 36 3.3 GJ 1032 2.5 0.4 Links are drawn between each star and its two closest neighbors. Gl 12 NN 3056 0.9 Gl 86 1.9 NN 3210 5.6 BD-09°431, a star with human-habitable planets 150 light years from Sol was arbitrarily chosen as the Zork homeworld. 1.4 3.1 Kappa Fornacis 1.9 GJ 1044 Wo 9061 B 0.6 53 Chi Ceti 2.2 2.3 0.6 1.7 2.0 1.3 Neutral zone stars are within 30 light years of a point exactly between Sol and Zork. 2.2 GJ 1048 1.7 Use this map to plot the expansion of each empire, colonized stars, battle fronts, and the location of other races. GJ 1026 0.8 GJ 1026 B 2.8 1.6 1.4 1.2 2.8 0.9 Gl 87 Gl 114.1 2.3 1.9 NN 3128 Gl 131 4.5 Hip 11439 2.0 2.7 Gl 84.1 Gl 91.2 Winchell D. Chung jr. "Nyrath the nearly wise" [email protected] 2006 1.6 CC Eridani 2.6 2.3 2.0 NN 3127 2.9 NN 3133 1.5 Gl 91.2B NN 3145 http://www.projectrho.com/starmap.html 3.2 2.0 1.9 NN 3131 27 Tau 6 Eridani Gl 84.1B 2.1 1.9 4.5 Hip 7765 1.6 GJ 1037 NN 4333 2.2 4.5 Gl 70 4.3 BD+04°123 1.9 NN 3076 1.5 1.3 2.3 0.9 1.4 1.9 Gl 145 2.6 Gl 146 0.4 1.9 Hip 12961 4.5 Gl 88 EQ Pegasi 1.6 Gl 95 GJ 1060 1.0 3.9 GJ 1060 B 2.3 Spectral Class A Gl 73 1.7 NN 3129 Gl 896 B 3.7 1.8 2.3 4.3 6.3 1.7 1.4 2.3 107 Piscium 1.8 NN 3146 4.2 3.9 Within 30 light years of Sol 2.4 1.2 2.3 Gl 120.1 Gl 120.1C Spectral Class F 2.1 1.9 2.7 2.6 1.1 Gl 91 Gl 120.1B No Human Habitable Planets 2.0 2.0 NN 3149 B 76 Sigma Ceti NN 4247 3.2 BD+15°4733 2.3 1.9 3.8 4.5 Hip 13610 Within 30 light years of Zork Spectral Class G NN 3120 0.6 6 Beta Arietis Gl 908 GJ 1054 1.3 1.0 BD-15°447 3.7 NN 3135 2.1 Gl 84 2.3 Parsecs Parsecs Parsecs Gl 109 1.7 BD-05°5715 Neutral Zone Spectral Class K Hip 14589 11 Tau 3 Eridani Human Habitable Planets 2.3 2.3 2.5 1.4 Spectral Class M Gl 105 GJ 1054 B All Other HU Delphini 2.8 2.5 1.7 1.8 1.8 GJ 1057 NN 3192 0.9 Gl 117 NN 3196 2.8 Gl 105 B Gl 121.1 1.9 2.5 Gl 143.1 3.2 NN 3249 3.8 NN 3197 B Spectral Class Unknown 0.8 2.0 2.4 1.5 2.3 2.8 The Neutral Zone 1.5 2.9 Gl 831 2.3 Hip 17420 GJ 1276 1.7 GJ 1286 4.8 Gl 100 Gl 831 B NN 3189 NN 3228 Hip 7776 96 Kappa 1 Ceti 23 Delta Eridani 2.3 NN 3193 B 1.7 Gl 100 B 2.2 NN 3229 B GJ 1256 2.1 Gl 142 2.4 2.7 Gl 100 C 3.5 Gl 829 NN 3175 2.5 2.5 2.2 NN 3139 2.0 2.2 Gl 905 0.8 2.2 NN 3263 4.1 NN 4274 3.6 BD-12°327 3.1 3.9 GJ 1051 Hip 9404 3.3 Hip 6273 1.4 0.6 2.8 5.1 4.5 2.8 1.3 3.1 GJ 1065 2.0 NN 3306 1.3 BD-16°308 V1581 Cygni 61 Cygni A Krüÿer 60 Hip 103039 Gl 183 1.7 1.6 1.5 GX Andromedae GJ 1289 Gl 785 3.7 NN 3113 0.8 3.9 GJ 1245 B 61 Cygni B DO Cephei FK Aquarii Gl 78 5.2 Gl 56.1 2.3 BD-14°249 2.6 BD-17°247 GQ Andromedae 1.8 BD-16°328 NN 3049 1.3 1.7 5.2 Gl 867 B GJ 1001 1.6 Gl 57.1 4.2 1.8 1.8 AU Microscopii 3.3 2.9 5.7 1.4 1.9 3.0 3.9 1.9 Gl 57.1B 1.6 3.5 6.8 2.8 2.2 BD-16°214 1.5 2.4 1.8 GJ 1027 Gl 57.1C 4.6 Hip 7916 Gl 725 B 3.9 Gl 180 BD-11°916 2.1 NN 3103 4.2 4.1 Gl 445 EV Lacertae 4.3 BD+04°158 NN 3072 2.2 2.3 2.3 2.4 Gl 725 44 Chi Draconis 2.0 Gl 892 1.1 4.1 3.2 2.9 Gl 783 0.9 NN 4360 Gl 915 4.9 1.7 BD-10°324 3.4 BD-11°298 Hip 93449 2.7 NN 3331 4.0 BD-10°403 BD-14°373 NN 3223 1.8 4.6 4.7 1.3 2.1 Gl 783 B UV Ceti A 2.4 Gl 81.1B 1.8 5.8 2.4 1.2 1.7 18 Epsilon Eridani NN 3332 B 1.0 4.0 4.8 4.9 1.5 2.1 2.5 2.2 1.8 Hip 7580 UV Ceti B 3.4 2.7 1.4 1.9 1.4 NN 3064 37 Ceti Hip 9753 3.1 4.3 2.8 1.6 2.2 5.7 3.5 3.1 3.0 4.0 0.7 4.7 Gl 687 GJ 1221 1.3 1.6 Gl 75 30 Mu Cassiopeiae 24 Eta Cassiopeiae 2.3 3.3 BD-12°233 2.9 2.5 NN 4053 1.6 BD-12°165 Gl 54.2B 5.2 BD-14°299 1.4 47 Ceti Gl 53 B Gl 34 B Gl 884 GJ 2005 1.2 BD-21°259 5.1 58 Eridani NN 3235 2.7 1.6 3.0 Hip 8039 1.9 5.0 Gl 754 2.4 3.2 1.6 1.5 1.7 2.6 4.5 1.0 1.1 2.3 1.3 1.1 3.3 3.3 4.5 BD-10°349 2.8 BD-11°318 4.8 BD-06°316 1.8 2.8 1.3 1.9 2.3 2.2 4.5 2.4 5.2 Hip 6276 7.5 BD-08°326 1.0 Hip 15689 0.6 1.4 2.3 61 Sigma Draconis 1.7 Gl 809 GJ 1227 BD-07°256 4.4 Gl 48 1.7 Gl 169.1 TW Piscis Austrini 13 Gamma Leporis BD-05°138 4.1 Hip 9692 3.4 BD-13°321 2.1 Gl 51 2.4 NN 3378 1.1 0.9 Hip 114176 BD-09°241 5.2 2.4 Fomalhaut 1.4 Gl 141 1.2 Hip 17695 Gl 120 3.4 4.6 3.4 Gl 169.1B Gl 216 B GJ 2030 B 1.8 1.2 5.7 GJ 1253 52 Tau Ceti GJ 1058 Hip 11323 45 Theta Ceti 1.1 2.9 2.2 1.9 1.1 4.3 BD-09°431 1.0 40 Omicron 2 Eridani 1.5 1.5 0.9 2.3 1.7 2.0 3.6 1.2 4.5 1.7 NN 3380 40 Eridani B 3.5 5.3 2.7 86 Gamma Ceti 3.3 5.6 3.2 5.8 70 Ophiuchi Gl 832 1.5 Epsilon Indi 1.0 BD-21°1051 Gl 190 0.9 13 Ceti 5.7 BD-20°470 4.2 Hip 11324 5.0 Zork 2.0 Hip 85605 Gl 784 1.9 GJ 1005 GJ 1002 DY Eridani 0.9 Gl 106.1B BD-17°400 BD-19°479 0.8 Gl 702 B Gl 793 4.9 Gl 226 3.5 NN 3417 2.2 NN 3325 Gl 23 B 5.3 4.1 Hip 8548 BD-10°462 7.4 Gl 185 B 2.0 NN 3218 10 Tauri 3.8 Gl 155.1 6.1 BD+08°482 2.5 Gl 106.1C Homeworld 2.6 1.2 1.3 1.5 2.0 1.3 4.6 1.8 2.4 2.0 1.6 1.3 BD+01°131 Hip 3757 2.5 4.3 1.6 1.6 2.3 Gl 157 2.1 5.5 BD+01°299 5.0 BD-02°311 41 Arae Gl 618 Gl 83.1 NN 3289 2.5 NN 3259 2.0 2.0 BD-03°174 2.1 Gl 157 B 3.7 1.6 2.4 1.4 4.1 4.7 3.2 Gl 752 Gl 666 B Gl 618 B 2.2 Lacaille 8760 Lacaille 9352 1.3 2.3 2.7 BD-07°351 1.2 BD+45°2505 2.0 Gl 1 Hip 114110 Hip 8844 Gl 752 B Altair 1.3 1.8 1.9 Hip 13976 BD-01°184 3.8 1.4 Hip 20968 2.9 2.9 2.0 Gl 661 B 4.1 6.4 NN 3323 Gl 100.1 6.9 7.4 7.1 2.5 1.2 Gl 633 NN 3104 87 Mu Ceti 1.9 NN 3163 1.4 3.4 3.5 2.5 3.5 3.7 1.3 1.3 NN 3205 Hip 10215 1.3 2.2 BD-05°353 1.7 2.3 2.9 NN 3305 NN 3261 3.3 2.0 0.4 Van Maanen's Star 2.7 1.3 Gl 693 1.9 NN 3421 2.4 GJ 1105 4.1 4.1 Delta Pavonis EZ Aquarii 2.6 1.4 6.0 3.5 3.2 2.5 Hip 82724 2.5 Gl 680 3.4 2.2 2.5 5.7 NN 3256 NN 3184 Hip 8998 3.1 5.7 1.4 GJ 2034 BD+00°256 5.4 1.0 3.4 2.2 4.5 4.7 1.5 4.0 1.8 Gl 213 1.1 Gl 729 2.1 1.5 0.9 1.4 Gl 56.3 4.0 3.9 Gl 625 1.1 IL Aquarii 1.3 2.4 Hip 9560 5.5 BD-15°478 0.8 0.9 1.3 BD+11°231 5.7 NN 3160 3.8 Hip 10500 1.7 BD-10°507 2.4 Gl 588 2.5 NN 3142 Gl 56.3B 3.6 3.0 3.4 3.9 Gl 682 2.8 1.5 3.7 Zeta Tucanae NN 4285 1.7 Hip 33226 0.9 2.2 6.3 1.7 Gl 268 1.1 1.1 NN 3174 2.5 Wo 9073 B 1.9 Gl 251 3.3 1.7 2.7 1.2 NN 3247 0.6 GJ 1062 NN 3221 2.1 2.8 4.0 Hip 82725 BD-07°699 3.2 2.8 Hip 11218 NN 3991 BD+43°2796 2.5 2.3 2.1 1.8 82 Eridani Hip 8972 3.1 BD-01°293 3.9 Hip 9989 7.7 BD-09°497 5.9 BD-09°427 BD+33°2777 2.4 1.9 Barnard's Star 1.6 GJ 1041 4.9 4.5 0.6 Gl 98 NN 3252 2.7 NN 3379 2.7 NN 3180 2.4 3.3 2.7 1.4 Gl 98 B BD+05°336 2.3 7.2 Gl 66 Beta Hydri 2.8 3.9 1.7 Gl 570 1.9 1.8 NN 3250 GJ 1052 Wo 9067 B 7.6 2.3 1.4 1.9 3.4 5.9 5.1 1.3 4.3 2.9 p Eridani 1.0 1.3 1.1 1.4 BD-12°525 3.8 4.7 BD-05°484 1.7 1.0 1.8 2.5 1.4 BD-08°547 Gl 674 1.6 Proxima Centauri Sol 1.4 BD-00°315 1.8 2.1 2.3 1.0 2.0 BD-12°558 NN 3988 2.0 2.7 Gl 563.2B Gamma Pavonis Gl 223.2 NN 3224 1.5 4.5 3.0 2.5 NN 3959 NN 3976 BD+18°3421 Rigel Kentaurus A 1.3 1.0 1.6 3.5 112 Piscium Gl 563.2 1.6 1.3 3.8 Luyten's Star 3.1 BD-03°1123 NN 3173 NN 3211 1.7 1.6 Rigel Kentaurus B Terran 1 Pi 3 Orionis NN 3237 2.2 4.1 GJ 1055 84 Ceti 1.0 BD+00°444 NN 3172 Hip 6762 4.3 1.5 2.0 4.2 3.3 4.8 1.4 2.7 0.8 3.8 6.0 1.9 2.1 3.4 86 Mu Herculis Homeworld 1.9 6.4 5.9 8.4 3.9 Gl 745 1.5 3.4 1.9 0.8 3.5 Gl 695 B 1.1 1.1 2.0 BD-09°572 Gl 745 B FL Virginis A DX Cancri BD+01°410 BD-08°535 BD-06°524 4.0 2.2 1.3 2.1 1.9 BD-02°476 66 Ceti Gl 695 C BD-12°4523 Gl 54 Gl 877 FL Virginis B Gl 447 3.3 2.1 GJ 1061 Gl 150.1 0.9 Gl 150.1B 2.8 4.7 2.1 BD-04°426 Hip 11182 4.2 BD-01°316 5.2 GJ 1087 2.8 1.6 V577 Monocerotis A 3.5 BD+11°383 3.2 BD+01°543 NN 3171 2.0 Gl 106 1.4 1.3 2.0 1.8 1.6 2.0 1.5 NN 3877 1.2 0.4 2.3 4.3 4.1 2.6 2.0 3.2 V577 Monocerotis B 2.9 1.8 1.4 1.4 6.8 1.7 1.6 2.1 5.1 3.8 4.6 4.5 4.6 4.4 1.5 2.7 3 Eta Eridani Gl 747 GJ 1230 Gl 406 1.2 Lalande 21185 BD-21°1377 0.8 10 Rho 3 Eridani 1.6 2.8 BD-07°4003 1.3 1.4 1.6 NN 3208 2.0 BD-03°410 GJ 1230 B BD-11°3759 3.0 BD+15°2620 1.3 NN 3225 Gl 747 B NN 3622 1.2 3.4 1.5 3.7 1.5 3.0 5.0 2.8 1.6 3.1 Hip 84581 V1054 Ophiuchi NN 3158 2.4 1.4 GJ 1116 3.0 Hip 9603 BD-14°604 6.1 BD-06°594 BD+00°404 7.5 BD-03°415 Gl 644 B 1.2 Procyon Sirius 2.0 2.8 2.4 1.3 1.9 2.5 NN 3522 1.6 1.4 0.7 NN 3132 1.3 1.4 Gl 644 C 2.1 1.8 1.5 GJ 1116 B Gl 244 B 3.7 4.1 1.1 2.0 Gl 280 B 2.8 1.7 2.3 NN 3159 1.5 NN 3153 2.9 2.3 1.7 1.6 Hip 10416 2.5 Hip 11029 Vega 2.0 0.7 2.6 NN 3181 Gl 104 4.3 BD+25°613 2.4 NN 3232 1.8 NN 4063 Gl 595 1.6 GJ 1207 BD-20°4123 GJ 2097 Gl 412 Kapteyn's Star 2.4 3.4 3.0 2.9 1.6 AD Leonis 2.1 Gl 338 3.8 Hip 14124 2.2 3.4 Gl 402 2.4 Gl 300 3.1 1.0 Gl 643 3.2 WX Ursae Majoris Gl 338 B 3.8 Stars within 30 light years of Zork BD+05°3409 2.5 2.6 3.5 12 Ophiuchi BD+11°2576 1.7 3.7 Gl 176 1.0 1.6 2.3 2.0 1.2 2.0 2.0 YZ Canis Minoris Gl 203 BD+18°683 2.3 2.9 2.4 NN 3820 3.4 1.8 BD+21°652 13 Zeta Eridani 2.1 14 Eridani Hip 13117 3.7 Hip 12856 Gl 518 0.4 2.0 BD-03°4233 Gl 465 2.2 GJ 1156 83 Epsilon Ceti 1.5 1.5 1.3 1.5 Groombridge 1618 NN 3454 1.2 NN 3304 BD+02°3312 1.9 3.1 1.3 Gl 408 0.9 NN 3155 1.7 BD-07°410 Gl 105.4B 1.9 1.8 1.1 1.9 36 Ophiuchi 3.9 BD-05°1844 1.9 2.0 1.7 61 Virginis Gl 299
Recommended publications
  • 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

    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.
  • FY08 Technical Papers by GSMTPO Staff

    FY08 Technical Papers by GSMTPO Staff

    AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................
  • Naming the Extrasolar Planets

    Naming the Extrasolar Planets

    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
  • Temperature-Spectral Class-Color Index Relationships for Main

    Temperature-Spectral Class-Color Index Relationships for Main

    ASTRONOMY SURVIVAL NOTEBOOK Stellar Evolution SESSION FOURTEEN: THE EVOLUTION OF STARS Approximate Characteristics of Several Types of MAIN SEQUENCE STARS Mass in Contraction Surface Luminosity M Years on Radius Class Comparison to Zero Age Temp. compared Absolute Main in to Sun Main Sequence (K) to sun Magnitude Sequence suns Not well known O6 29.5 10 Th 45,000 140,000 -4.0 2 M 6.2 mid blue super g O9 22.6 100 Th 37,800 55,000 -3.6 4 M 4.7 late blue super g B2 10.0 400 Th 21,000 3,190 -1.9 30 M 4.3 early B5 5.46 1 M 15,200 380 -0.4 140 M 2.8 mid A0 2.48 4 M 9,600 24 +1.5 1B 1.8 early A7 1.86 10 M 7,920 8.8 +2.4 2 B 1.6 late F2 1.46 15 M 7,050 3.8 +3.8 4 B 1.3 early G2 1.00 20 M 5,800 1.0 +4.83 10 B 1.0 early sun K7 0.53 40 M 4,000 0.11 +8.1 50 B 0.7 late M8 0.17 100 M 2,700 0.0020 +14.4 840B 0.2 late minimum 2 Jupiters Temperature-Spectral Class-Color Index Relationships for Main-Sequence Stars Temp 54,000 K 29,200 K 9,600 K 7,350 K 6,050 K 5,240 K 3,750 K | | | | | | | Sp Class O5 B0 A0 F0 G0 K0 M0 Co Index (UBV) -0.33 -0.30 -0.02 +0.30 +0.58 +0.81 +1.40 1.
  • Jjmonl 1810.Pmd

    Jjmonl 1810.Pmd

    alactic Observer John J. McCarthy Observatory G Volume 11, No. 10 October 2018 Halloween spook See page 19 for more information The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue INTERNATIONAL OBSERVE THE MOON NIGHT .......................... 3 INTERNATIONAL SPACE STATION/IRIDIUM SATELLITES .............. 18 INOMN HIGHLIGHT, MARE HUMORUM SOLAR ACTIVITY ................................................................ 18 AND GASSENDI CRATER .................................................. 5 NASA'S GLOBAL CLIMATE CHANGE ................................... 18 LUNAR ICE ........................................................................
  • Arxiv:0809.1275V2

    Arxiv:0809.1275V2

    How eccentric orbital solutions can hide planetary systems in 2:1 resonant orbits Guillem Anglada-Escud´e1, Mercedes L´opez-Morales1,2, John E. Chambers1 [email protected], [email protected], [email protected] ABSTRACT The Doppler technique measures the reflex radial motion of a star induced by the presence of companions and is the most successful method to detect ex- oplanets. If several planets are present, their signals will appear combined in the radial motion of the star, leading to potential misinterpretations of the data. Specifically, two planets in 2:1 resonant orbits can mimic the signal of a sin- gle planet in an eccentric orbit. We quantify the implications of this statistical degeneracy for a representative sample of the reported single exoplanets with available datasets, finding that 1) around 35% percent of the published eccentric one-planet solutions are statistically indistinguishible from planetary systems in 2:1 orbital resonance, 2) another 40% cannot be statistically distinguished from a circular orbital solution and 3) planets with masses comparable to Earth could be hidden in known orbital solutions of eccentric super-Earths and Neptune mass planets. Subject headings: Exoplanets – Orbital dynamics – Planet detection – Doppler method arXiv:0809.1275v2 [astro-ph] 25 Nov 2009 Introduction Most of the +300 exoplanets found to date have been discovered using the Doppler tech- nique, which measures the reflex motion of the host star induced by the planets (Mayor & Queloz 1995; Marcy & Butler 1996). The diverse characteristics of these exoplanets are somewhat surprising. Many of them are similar in mass to Jupiter, but orbit much closer to their 1Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Rd.
  • Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆

    Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆

    A&A 565, A15 (2014) Astronomy DOI: 10.1051/0004-6361/201323058 & c ESO 2014 Astrophysics Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel J. P. Marshall1,2, A. Moro-Martín3,4, C. Eiroa1, G. Kennedy5,A.Mora6, B. Sibthorpe7, J.-F. Lestrade8, J. Maldonado1,9, J. Sanz-Forcada10,M.C.Wyatt5,B.Matthews11,12,J.Horner2,13,14, B. Montesinos10,G.Bryden15, C. del Burgo16,J.S.Greaves17,R.J.Ivison18,19, G. Meeus1, G. Olofsson20, G. L. Pilbratt21, and G. J. White22,23 (Affiliations can be found after the references) Received 15 November 2013 / Accepted 6 March 2014 ABSTRACT Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 μm with the sensitiv- ity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system’s Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis.
  • An October 2003 Amateur Observation of HD 209458B

    An October 2003 Amateur Observation of HD 209458B

    Tsunami 3-2004 A Shadow over Oxie Anders Nyholm A shadow over Oxie – An October 2003 amateur observation of HD 209458b Anders Nyholm Rymdgymnasiet Kiruna, Sweden April 2004 Tsunami 3-2004 A Shadow over Oxie Anders Nyholm Abstract This paper describes a photometry observation by an amateur astronomer of a transit of the extrasolar planet HD 209458b across its star on the 26th of October 2003. A description of the telescope, CCD imager, software and method used is provided. The preparations leading to the transit observation are described, along with a chronology. The results of the observation (in the form of a time-magnitude diagram) is reproduced, investigated and discussed. It is concluded that the HD 209458b transit most probably was observed. A number of less successful attempts at observing HD 209458b transits in August and October 2003 are also described. A general introduction describes the development in astronomy leading to observations of extrasolar planets in general and amateur observations of extrasolar planets in particular. Tsunami 3-2004 A Shadow over Oxie Anders Nyholm Contents 1. Introduction 3 2. Background 3 2.1 Transit pre-history: Mercury and Venus 3 2.2 Extrasolar planets: a brief history 4 2.3 Early photometry proposals 6 2.4 HD 209458b: discovery and study 6 2.5 Stellar characteristics of HD 209458 6 2.6 Characteristics of HD 209458b 7 3. Observations 7 3.1 Observatory, equipment and software 7 3.2 Test observation of SAO 42275 on the 14th of April 2003 7 3.3 Selection of candidate transits 7 3.4 Test observation and transit observation attempts in August 2003 8 3.5 Transit observation attempt on the 12th of October 2003 8 3.6 Transit observation attempt on the 26th of October 2003 8 4.
  • Coronal Activity Cycles in 61 Cygni

    Coronal Activity Cycles in 61 Cygni

    A&A 460, 261–267 (2006) Astronomy DOI: 10.1051/0004-6361:20065459 & c ESO 2006 Astrophysics Coronal activity cycles in 61 Cygni A. Hempelmann1, J. Robrade1,J.H.M.M.Schmitt1,F.Favata2,S.L.Baliunas3, and J. C. Hall4 1 Universität Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [email protected] 2 Astrophysics Division – Research and Science Support Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands 3 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA 4 Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA Received 19 April 2006 / Accepted 25 July 2006 ABSTRACT Context. While the existence of stellar analogues of the 11 years solar activity cycle is proven for dozens of stars from optical observations of chromospheric activity, the observation of clearly cyclical coronal activity is still in its infancy. Aims. In this paper, long-term X-ray monitoring of the binary 61 Cygni is used to investigate possible coronal activity cycles in moderately active stars. Methods. We are monitoring both stellar components, a K5V (A) and a K7V (B) star, of 61 Cyg with XMM-Newton. The first four years of these observations are combined with ROSAT HRI observations of an earlier monitoring campaign. The X-ray light curves are compared with the long-term monitoring of chromospheric activity, as measured by the Mt.Wilson CaII H+K S -index. Results. Besides the observation of variability on short time scales, long-term variations of the X-ray activity are clearly present. For 61 Cyg A we find a coronal cycle which clearly reflects the well-known and distinct chromospheric activity cycle.
  • MYLES GASKIN Going out in Style HUSKY PICKS for HOLIDAY TRAVELS

    MYLES GASKIN Going out in Style HUSKY PICKS for HOLIDAY TRAVELS

    THE UNIVERSITY OF WASHINGTON ALUMNI MAGAZINE DEC 18 THE GREATEST RUNNING BACK IN HUSKY HISTORY MYLES GASKIN Going Out In Style HUSKY PICKS FOR HOLIDAY TRAVELS Columbia Flannel Long Sleeve Shirt Sport Noir Sheen Tote fanatics.com shop.littlearth.com Knit Hat zhats.com String Pack logobrands.com Outerstuff Girls' Washington W Fame Hoodie ubookstore.com Travel Backpack sportsluggage.com Wheeled Carry-on Duffl e Hardcase Carry-on Spinner Travel Pillows Plush Teddy Bear sportsluggage.com pegasussports.com huskyteamstore.com I GIVE BECAUSE photographed in cooperation with UW partner Alaska Airlines COLLEGE CHANGES LIVES Merisa H.W. Lawyer, mother, champion Dawg Pack Pup Size Road Rest Dawg Wash Your Dawg (or cat) will enjoy the Travel prepared with this Arrive awake and alert. This Stay fresh on the go with this journey in one of these two stylish to-go size 6-piece fan kit frosty tipped, high-pile Sherpa Husky travel case/toiletry bag. in-cabin pet carriers. Lightweight of essential supplies— throw will keep you toasty warm. Durable microfi ber and interior polyester, a removable washable lip balm, hand sanitizer, wet Thick Husky purple trim and and exterior zippered pockets JOIN ME pad, and mesh ventilation panels wipes, SPF-30 sunscreen, logo patch confi rm that you’re make it handy for headphones, make these comfortable quarters for peppermints and nail clippers. a happy napping Dawg. jewelry, and charging cords, too. uw.edu/boundless #beboundless all pets (except Cougs and Ducks). amazon.com ubookstore.com amazon.com sportsluggage.com REAL DAWGS WEAR PURPLE WearPurple 2 COLUMNS MAGAZINE DEC 2 0 1 8 realdawgswearpurple HuskyPicks_winter.indd 1 11/5/18 11:53 AM Full Page Ad Template | Live Area 7.75" x 10.25" | Trim Size 8.375" x 10.875" | Bleed Size 8.875" x 11.375" Seattle.
  • Across the Atlantic: Canada's MOST

    Across the Atlantic: Canada's MOST

    The CoRoT Legacy Book c The authors, 2016 DOI: 10.1051/978-2-7598-1876-1.c014 I.4 Across the Atlantic: Canada’s MOST J. M. Matthews Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, V6T 1Z1 Canada contractors were Dynacon, and CRESTech (Centre for 1. Windows of opportunity Research in Earth & Space Technology). John Pazder be- In the mid-1990s, it seemed like the only way Canadian came the optics designer and Peter Ceravolo would fabri- astronomers could have direct access to space-based ultra- cate the main optics. precise photometry for asteroseismology was to be a minor The project was renamed MOST, for Microvariabil- partner in a European satellite mission. In fact, with this ity & Oscillations of STars/Microvariabilit´eet Oscillations in mind, in 1996 Jaymie Matthews (University of British STellaire. Its original scientific objectives were: (1) astero- Columbia) submitted an unsolicited proposal to the Cana- seismology of solar-type stars; (2) asteroseismology of roAp dian Space Agency for Canada to participate in Eddington (rapidly oscillating Ap) stars; (3) characterization of Wolf- at a level of a few Can$M. Rayet star winds and search for pulsations; and (4) mea- Then two unexpected windows opened right after one surement of exoplanet albedo. another. MOST won the Phase A competition and was selected The first window was built by aerospace engineer Kieran to be Canada's first microsatellite and first space telescope. Carroll and opened by astronomer Slavek Rucinski. Rucin- ski attended a talk by Carroll whose company, Dynacon Inc. had developed a new Attitude Control System (ACS).
  • Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B

    Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B

    Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis,