Planet Hunters IX. KIC 8462852-where's the flux?

被引：171

作者：

Boyajian, T. S. ^{[1
]}

LaCourse, D. M. ^{[2
]}

Rappaport, S. A. ^{[3
,4
]}

Fabrycky, D. ^{[5
]}

Fischer, D. A. ^{[1
]}

Gandolfi, D. ^{[6
,7
]}

Kennedy, G. M. ^{[8
]}

Korhonen, H. ^{[9
,10
]}

Liu, M. C. ^{[11
]}

Moor, A. ^{[12
]}

Olah, K. ^{[12
]}

Vida, K. ^{[12
]}

Wyatt, M. C. ^{[8
]}

Best, W. M. J. ^{[11
]}

Brewer, J. ^{[1
]}

Ciesla, F. ^{[13
]}

Csak, B. ^{[14
]}

Deeg, H. J. ^{[15
,16
]}

Dupuy, T. J. ^{[17
]}

Handler, G. ^{[18
]}

Heng, K. ^{[19
]}

Howell, S. B. ^{[20
]}

Ishikawa, S. T. ^{[21
]}

Kovacs, J. ^{[14
]}

Kozakis, T. ^{[22
]}

Kriskovics, L. ^{[12
]}

Lehtinen, J. ^{[23
]}

Lintott, C. ^{[24
]}

Lynn, S. ^{[25
]}

Nespral, D. ^{[15
]}

Nikbakhsh, S. ^{[23
,26
]}

Schawinski, K. ^{[27
]}

Schmitt, J. R. ^{[1
]}

Smith, A. M. ^{[28
]}

Szabo, Gy. ^{[12
,29
]}

Szabo, R. ^{[12
]}

Viuho, J. ^{[23
]}

Wang, J. ^{[1
,30
]}

Weiksnar, A. ^{[21
]}

Bosch, M. ^{[2
]}

Connors, J. L. ^{[2
]}

Goodman, S. ^{[2
]}

Green, G. ^{[2
]}

Hoekstra, A. J. ^{[2
]}

Jebson, T. ^{[2
]}

Jek, K. J. ^{[2
]}

Omohundro, M. R. ^{[2
]}

Schwengeler, H. M. ^{[2
]}

Szewczyk, A. ^{[2
]}

机构：

[1] Yale Univ, Dept Astron, New Haven, CT 06511 USA

[2] Amateur Astronomer, Helsinki, Finland

[3] MIT, Dept Phys, Cambridge, MA 02139 USA

[4] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[5] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA

[6] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy

[7] Heidelberg Univ, Zentrum Astron, Landessternwarte Konigstuhl, Konigstuhl 12, D-69117 Heidelberg, Germany

[8] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[9] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Turku, Finland

[10] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark

[11] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

[12] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Th M ut 15 17, H-1121 Budapest, Hungary

[13] Univ Chicago, Dept Geophys Sci, 5734 South Ellis Ave, Chicago, IL 60637 USA

[14] ELTE Gothard Astrophys Observ, Szent Imre Herceg Ut 112, H-9704 Szombathely, Hungary

[15] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 Tenerife, Spain

[16] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain

[17] Univ Texas Austin, Dept Astron, 2515 Speedway C1400, Austin, TX 78712 USA

[18] Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland

[19] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland

[20] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[21] Adler Planetarium, Dept Citizen Sci, 1300 S Lake Shore Dr, Chicago, IL 60605 USA

[22] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA

[23] Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland

[24] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[25] CartoDB, 247 Ctr St, New York, NY 10013 USA

[26] Finnish Meteorol Inst, POB 503, FI-00101 Helsinki, Finland

[27] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland

[28] GitHub Inc, 88 Colin P Kelly Jr St, San Francisco, CA 94107 USA

[29] Gothard Lendulet Res Team, Szent Imre Herceg Ut 112, H-9704 Szombathely, Hungary

[30] CALTECH, Pasadena, CA 91109 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 457卷 / 04期

基金：

瑞士国家科学基金会; 美国国家航空航天局;

关键词：

comets: general; planets and satellites: dynamical evolution and stability; stars: activity; stars: individual: KIC 8462852; stars: peculiar; INFRARED FILTER SET; BETA-PICTORIS; SOLAR-SYSTEM; DEBRIS DISKS; IRREGULAR SATELLITES; CIRCUMSTELLAR DISK; INTRINSIC COLORS; MAIN-SEQUENCE; ARCHIVE DATA; AA TAURI;

D O I：

10.1093/mnras/stw218

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Over the duration of the Kepler mission, KIC 8462852 was observed to undergo irregularly shaped, aperiodic dips in flux of up to similar to 20 per cent. The dipping activity can last for between 5 and 80 d. We characterize the object with high-resolution spectroscopy, spectral energy distribution fitting, radial velocity measurements, high-resolution imaging, and Fourier analyses of the Kepler light curve. We determine that KIC 8462852 is a typical main-sequence F3 V star that exhibits no significant IR excess, and has no very close interacting companions. In this paper, we describe various scenarios to explain the dipping events observed in the Kepler light curve. We confirm that the dipping signals in the data are not caused by any instrumental or data processing artefact, and thus are astrophysical in origin. We construct scenario-independent constraints on the size and location of a body in the system that are needed to reproduce the observations. We deliberate over several assorted stellar and circumstellar astrophysical scenarios, most of which have problems explaining the data in hand. By considering the observational constraints on dust clumps in orbit around a normal main-sequence star, we conclude that the scenario most consistent with the data in hand is the passage of a family of exocomet or planetesimal fragments, all of which are associated with a single previous break-up event, possibly caused by tidal disruption or thermal processing. The minimum total mass associated with these fragments likely exceeds 10(-6) M-circle plus, corresponding to an original rocky body of > 100 km in diameter. We discuss the necessity of future observations to help interpret the system.

引用

页码：3988 / 4004

页数：17

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