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A Absorptivity, 642, 682 Abundance(S), 339, 388, 389, 408

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Index A momentum, 354, 383–385, 443–445, 475, Absorptivity, 642, 682 479, 510, 589, 607, 681, 701, 778 Abundance(s), 339, 388, 389, 408, 410, 484, resolution, 686 485, 491, 509, 541, 560, 561, 616, velocity/velocities, 349, 350, 354, 570, 605 619, 621, 648, 654, 658–661, 665, Apollonius of Myndus, 598 667, 668, 670, 673, 676, 780 Aquinas, T., 598 Acetonitrile (CH3CN), 561, 619 Archaeomagnetic data, 423 Acetylene (C2H2), 559, 560, 562 Ariel (satellite, Uranus I), 523, 527, 532, Adams, J.C., 492, 493, 582 533, 564 Adams-Williamson equation, 494 albedo, 564 Adiabatic Aristotle, 598, 599 convection, 344, 345 Artemis, 648 lapse rate, 348, 368, 369, 375, 385 Asteroid(s) (general) pressure-density relation, 344 albedo(s), 683, 686–688, 696, 700 processes, 345 densities, 639, 689–690 Adoration of Magi, 610, 612 dimension(s), 686–690 Adrastea (satellite, Jupiter XV), 524, 529, 572 double, 689 Airy, G.B., 492 inner solar system plot, 678, 681, 690 Albedo masses, 686–690 bolometric, 338, 477, 636, 642, 687, 780 nomenclature, 648–649, 677–681 bond, 477, 516, 627, 747, 772, 780 orbital properties geometric (visual), 477, 564, 581 families, 681–685 Alfve´n waves, 460 Kirkwood gaps, 582, 678, 695, 697 Aluminum isotopes, 694 outer solar system plot, 588–590, 603 Alvarez, L., 668 radii, 688 Amalthea (satellite, Jupiter V), 355, 529, rotations, 688, 700 537, 572 thermal emissions, 697 Ambipolar diffusion, 402, 703 Asteroid mill, 639, 676, 769 American Meteor Society, 637, 638 Asteroids (individual) Amidogen radical (NH2), (2101) Adonis, 683 Ammonia (NH3), 348, 391, 480, 481, 483, (1221) Amor, 681, 690 485, 512, 558, 560, 619, 625, (3554) Amun, 683 627, 756 (1943) Anteros, 681 Ammonium hydrosulfide (NH4SH), 481, 483 (2061) Anza, 681 Anaxagoras of Clazomenae, 598 (1862) Apollo, 683, 684, 698 Angular (197) Ariete, 689 diameter(s), 493, 686 (2062) Aten, 683 E.F. Milone and W.J.F. Wilson, Solar System Astrophysics: Planetary 797 Atmospheres and the Outer Solar System, Astronomy and Astrophysics Library, DOI 10.1007/978-1-4614-9090-6, © Springer Science+Business Media New York 2014 798 Index Asteroids (individual) (cont.) eddy/eddies, 363–365, 384 (1865) Cerberus, 683 Ferrel cell(s), 362–363, 378, 385 (1) Ceres, 676–677, 689 global, 360–367 (2060) Chiron, 627, 684 Hadley cell(s), 361–362, 378–380, 384, (1864) Daedalus, 683 480, 555, 558 (136199) Eris, 528, 690 meridional, 363–366, 378–381, 384, (433) Eros, 681, 683, 690, 691, 698 555, 556 (951) Gaspra, 689 parasitic cell(s), 363 (2340) Hathor, 683 polar cell(s), 362–363 (624) Hektor (Hector), 689 thermal, 357–358, 362 (2212) Hephaistos, 683 wave motion(s), 365 (944) Hidalgo, 627, 684, 699 zonal, 365, 366, 380–385, 555 (1566) Icarus, 683 constituent(s), 337–340, 371, 372, 479, 560, (243) Ida, 689 764, 773 (3) Juno, 690, 691 comparative, 387 (2) Pallas, 677, 678, 687, 689–691, 698 convection, 344, 345, 369, 388, 483 1989 PB, diffusion, 386–389, 484, 496 (3200) Phaethon, 631, 683 diffusion time, 388, 496 (5145) Pholus, 627, 685 diffusive equilibrium, 388 (1915) Quetzalcoatl, 681 Earth (5381) Sekhmet, 681 average lapse rate, 368 (2608) Seneca, 681 circulation, 357, 361, 377, 378, 555 2004 VB61, 681 composition, 387, 781 (4) Vesta, 653, 689–696 cyclones, 383, 384 2004 WC1, 683 diffusion time, 388 2004 WS2, 683 dry adiabatic lapse rate (DALR), Asteroids (types) 368, 375 Amor(s), 681, 690 escape mechanisms, 411–416 Apollo(s), 683, 684, 698 exosphere, 371, 411, 415, 467, 545 Aten(s), 683 heterosphere, 389 Centaur(s), 589, 609, 627, 680 homosphere, 389 Cubewano(s), 681 hurricane(s), 354, 375, 385 excited/hot objects, 685 lapse rate, 372 Flora family, 681, 682 mesopause, 370, 389 Hilda family, 679, 681, 684, 698 mesosphere, 369–370 Koronis family, 681, 682, 689 mixing time, 388, 389 Kuiper Belt objects (KBOs) ozone, 367 classical/cold, 685 pressure scale height, 357, 371, excited/hot, 685 372, 449 main belt, 642, 678, 679, 681, 690, 693, Rossby number, 377, 378, 383 697, 759 saturated adiabatic lapse rate Plutino(s), 568, 589, 680, 681, 685, 759 (SALR), 369 scattered population, 626, 628, 685, 779 stratosphere, 369–370 trans-Neptunian object(s) (TNOs), 568, superrotation, 384, 385 589, 685, 690, 759 thermal structure, 368 eccentricities vs. semi-major axes, 685 thermosphere, 370, 371, 373, 376 Trojan(s) & Greek(s), 548, 677, 679, 681, tropopause, 365 684, 690, 699 troposphere, 367–369, 372, 386, Astronomical unit (au), 339, 601, 609, 769 393, 556 Atlas (satellite, Saturn XV), 526, 530, 576 winds, 361, 365, 372, 380, 382, 384, Atmosphere/atmospheric 385, 413, 416, 423, 424, 440, 448, air mass(es), 364, 365 455, 464, 467, 480, 503, 509, 510, circulation(s) 512, 555, 558 Index 799 eddy/eddies, 356, 363–364, 380, 384 seeing, 686 effects on heat transport, 363, 365 structure, 340–349, 368, 371, 375, 478, escape mechanisms, 411–416 483–486, 490, 497 exobase, 411–413, 446, 467, 547 subtropical fronts, 365, 366 heterosphere, 389 thermal inertia, 371, 375, 378, 385–386 homopause, 389 tides, 439, 586, 648 homosphere, 389 total density scale height, 412 isobars, 356, 359 Uranus, 483, 485, 490–491, 493, 496 isotherm(s), 357, 358, 360, 380, 381 Venus jet stream(s), 365–367, 374, 380, 480 circulation, 377, 378, 381–385 Jupiter composition, 387 belts, 480, 482, 582, 678, 679, 681, cryosphere, 376, 412 695, 779 cyclostrophic balance, 382–384, 555 brown barges, 480, 481 exobase altitude, 412 Great Red Spot (GRS), 480–482, 485, 493 haze layer, 374, 381 helium deficiency, 496 homopause, 389 mean molecular weight, 343, 478, 479 lapse rate, 372, 375 pressure scale height, 765 mesosphere, 375, 376, 555 white spot(s), 538 Rossby number, 380, 382 winds, 480, 481, 500, 503, 509–511, 514 stratomesosphere, zones, 480–483, 487, 503, 509, 543, superrotation, 381–382, 384, 385 587, 628 temperature, 349, 367, 372, 375, 376, Mars 386, 393, 394, 412–414, 463, 555 averaged temperatures, 381 thermal structure, 368, 375 circulation, 377, 378, 380–381, 385 thermosphere, 375–377 composition, 387, 653, 666 troposphere, 375, 556 dust devils, 372, 373 Aurora(e), 434–436, 441, 449, 452, 454, 456, homopause, 389 469, 485, 488, 503, 504 ionosphere, 409–410, 467 Auroral oval, 416, 449, 450, 452–454, 456, lapse rate, 372, 373 488, 503, 504, 507, 515, 584 mixing rate, Avogadro’s number, 343, 346 mixing ratio(s), 349, 407 Rossby number, 377, 378 stratomesosphere, 371 B thermal structure, 368, 371 Bacon, R., 598 thermosphere, 371, 373, 376 Baroclinic instability, 363 troposphere, 371–373, 375, 407 Bayeaux tapestry, 610, 612 meridional cross-section(s), 365, 366 Benzene (C6H6), 562 mixing, 386–389 Bessel, F.W., 601 mixing ratio, 349, 391, 407 Bielids, 631 mixing time, 388, 389 Bipolar outflow(s), 701, 703 Neptune, 395, 483, 492–494 Birkeland currents, 453, 454 pressure Bode, J.E., 676 baroclinic instabilities, 363 Bolide(s), 631, 632, 635, 637, 638, 647, 659 gradient(s), 342, 353–357, 359, 360, Bolometer, 688 376, 382, 383, 479 Boltzmann constant, 337, 338, 411, 702 high/low, 356, 358, 359, 362, 364, Borelli, G., 600 383, 481 Boundary current, 440, 441, 448, 451, 462, refractive index, 344, 418, 421, 423 464, 510 Saturn Bradley, J., 490 features, 487, 490 Brahe,T., 598–600 structure, 486–489, 497, 515, 582 Breccia(s) winds, 488, 509, 513, 515 anorthositic, 666 800 Index Breccia(s) (cont.) Carbon monoxide (CO), 347, 372, 387, 407, basaltic, 666 408, 412, 483, 547, 560, 565, 568, genomict, 663 619, 620, 651, 653, 657, 659, 661, monomict, 655, 663 698, 760, 766 polymict, 655, 663 Cardan, Jerome (Cardano, Girolamo), 598 regolith, 663, 664, 666 Cassini/Cassini’s Division, 575, 576, 585 Bright Star Catalog, 714 Cassini, J.-D., 575 Brown dwarf desert, 723, 740, 742, 777 Cassini state, 489 Brown dwarf(s), general Catalog of Meteorites, 649 definition, 758–761 Centaurs, 589, 609, 627, 680, 684, 685 detection techniques, 723, 743, 744, 755 Ceres (asteroid dwarf planet), 522, 568, evolution, 778 589, 759 origins, 776–781 Chaeremon the Stoic, 597 spectral characteristics, 650, 681, 693, Chalcophilic elements, 658 695, 760 Challis, J., 492 Brown dwarf(s), individual Chaotic variation, 627, 697 AB Pic B, 756 Chapman-Ferraro current, 440, 462 Cha 110913-773444, 756 Charge-exchange reactions, 467, 506, 514 GD 165 B, 760 Charon (satellite, Pluto I) Gliese 229 B, 760 atmosphere, 528, 533, 568, 570 GQ Lupi B, 322 composition, 478 HD 137510 B, 753 discovery, 528, 568, 589 HD 168443 C, 753 orbit/orbital 2MASS J0535-0546 A, 760 elements, 477, 528, 549, 627 2MASS J1207-3932 a, 755 properties, 475, 535, 570, 706, 723 OGLE-TR-109B, 763 spin-orbit resonance, 568 Ross 458 C, 761 Chinook, 395 Brownlee particles, 620, 639 Chiron (asteroid), 589, 609, 625, 627, Brunt-Va¨isa¨la¨ frequency, 386 684, 685 Chladni, E.F.F., 647 Chondrites. See under Meteorites C Chondrules Calcium-aluminum inclusion(s) (CAI), 620, composition, 652, 657, 658, 660 640, 657–660, 662, 676 origin, 658 Callisto (satellite, Jupiter IV) CHON particles, 620 atmosphere, 545, 547 CH radical, 562 domed crater(s), 543, 547 Circulation interior, 555 Ferrel cell(s), 362–363 magnetic field, 545 global, 360–367 moment of inertia, 545, 553 Hadley cell(s), 361–363, 378 ringed plain(s), 541, 545 parasitic cell(s), 363 sub-surface ocean, 555, 779 polar cell(s), 362–363 surface feature(s), 358, 539 Clairaut, A.-C., 601 Valhalla (ringed plain), 545, 546 CN radical, 614 Campbell, W.W., 575 Coefficient Capture mechanisms, 535 ablation, 635 Carbon black, 627 drag, 634 Carbon dioxide (CO2), 348, 367, 370, 372, 373, Comet(s)/cometary 375, 376, 378, 387, 389–391, 393, attrition, 628 407, 408, 410, 411, 413, 469, 512, coma, 613, 615, 616,
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    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
  • A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?

    A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?

    geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3].
  • Exoplanet Meteorology: Characterizing the Atmospheres Of

    Exoplanet Meteorology: Characterizing the Atmospheres Of

    Exoplanet Meteorology: Characterizing the Atmospheres of Directly Imaged Sub-Stellar Objects by Abhijith Rajan A Dissertation Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy Approved April 2017 by the Graduate Supervisory Committee: Jennifer Patience, Co-Chair Patrick Young, Co-Chair Paul Scowen Nathaniel Butler Evgenya Shkolnik ARIZONA STATE UNIVERSITY May 2017 ©2017 Abhijith Rajan All Rights Reserved ABSTRACT The field of exoplanet science has matured over the past two decades with over 3500 confirmed exoplanets. However, many fundamental questions regarding the composition, and formation mechanism remain unanswered. Atmospheres are a window into the properties of a planet, and spectroscopic studies can help resolve many of these questions. For the first part of my dissertation, I participated in two studies of the atmospheres of brown dwarfs to search for weather variations. To understand the evolution of weather on brown dwarfs we conducted a multi- epoch study monitoring four cool brown dwarfs to search for photometric variability. These cool brown dwarfs are predicted to have salt and sulfide clouds condensing in their upper atmosphere and we detected one high amplitude variable. Combining observations for all T5 and later brown dwarfs we note a possible correlation between variability and cloud opacity. For the second half of my thesis, I focused on characterizing the atmospheres of directly imaged exoplanets. In the first study Hubble Space Telescope data on HR8799, in wavelengths unobservable from the ground, provide constraints on the presence of clouds in the outer planets. Next, I present research done in collaboration with the Gemini Planet Imager Exoplanet Survey (GPIES) team including an exploration of the instrument contrast against environmental parameters, and an examination of the environment of the planet in the HD 106906 system.