Transiting exoplanets from the CoRoT space mission XXVIII. CoRoT-33b, an object in the brown dwarf desert with 2:3 commensurability with its host star

被引：50

作者：

Csizmadia, Sz ^{[1
]}

Hatzes, A. ^{[2
]}

Gandolfi, D. ^{[3
,4
]}

Deleuil, M. ^{[5
]}

Bouchy, F. ^{[5
]}

Fridlund, M. ^{[6
,7
,8
]}

Szabados, L. ^{[9
]}

Parviainen, H. ^{[10
]}

Cabrera, J. ^{[1
]}

Aigrain, S. ^{[11
]}

Alonso, R. ^{[12
,13
]}

Almenara, J. -M. ^{[5
]}

Baglin, A. ^{[14
]}

Borde, P. ^{[15
,16
]}

Bonomo, A. S. ^{[17
]}

Deeg, H. J. ^{[12
,13
]}

Diaz, R. F. ^{[18
]}

Erikson, A. ^{[1
]}

Ferraz-Mello, S. ^{[19
]}

Tadeu dos Santos, M. ^{[19
]}

Guenther, E. W. ^{[2
]}

Guillot, T. ^{[20
]}

Grziwa, S. ^{[21
]}

Hebrard, G. ^{[22
]}

Klagyivik, P. ^{[12
,13
]}

Ollivier, M. ^{[23
]}

Paetzold, M. ^{[21
]}

Rauer, H. ^{[1
,24
]}

Rouan, D. ^{[14
]}

Santerne, A. ^{[25
]}

Schneider, J. ^{[26
]}

Mazeh, T. ^{[27
]}

Wuchterl, G. ^{[2
]}

Carpano, S. ^{[28
]}

Ofir, A. ^{[29
]}

机构：

[1] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany

[2] Thuringer Landessternwarte, D-07778 Tautenburg, Germany

[3] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy

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

[5] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille UMR 7326, F-13388 Marseille, France

[6] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[7] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[8] Chalmers Univ Technol, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden

[9] Hungarian Acad Sci, Konkoly Observ, MTA CSFK, Budapest, Hungary

[10] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England

[11] Univ Oxford, Dept Phys, Oxford OX1 3RH, England

[12] Inst Astrofis Canarias, Tenerife 38205, Spain

[13] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

[14] Univ Paris Diderot, UPMC, Observ Paris, LESIA,UMR CNRS 8109, F-92195 Meudon, France

[15] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France

[16] CNRS, F-33270 Floirac, France

[17] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, TO, Italy

[18] Univ Geneva, Observ Astron, CH-1290 Versoix, Switzerland

[19] IAG Univ Sao Paulo, BR-1226 Sao Paulo, Brazil

[20] Univ Nice Sophia Antipolis, CNRS UMR 6202, Observ Cote dAzur, F-06304 Nice 4, France

[21] Univ Cologne, Rhein Inst Umweltforsch, D-50931 Cologne, Germany

[22] Univ Paris 06, UMR CNRS 7095, Inst Astrophys Paris, F-75014 Paris, France

[23] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France

[24] TU Berlin, Ctr Astron & Astrophys, D-10623 Berlin, Germany

[25] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal

[26] Univ Paris Diderot, UMR CNRS 8102, Observ Paris, LUTH, F-92195 Meudon, France

[27] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-39040 Tel Aviv, Israel

[28] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[29] Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-76100 Rehovot, Israel

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 584卷

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

brown dwarfs; stars: rotation; eclipses; SOLAR-TYPE STARS; SOPHIE VELOCIMETRY; SHORT-PERIOD; DARKENING COEFFICIENTS; MODEL ATMOSPHERES; PLANET OCCURRENCE; LIGHT CURVES; MASS; COMPANIONS; CANDIDATES;

D O I：

10.1051/0004-6361/201526763

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the detection of a rare transiting brown dwarf with a mass of 59 M-Jup and radius of 1.1 R-Jup around the metal-rich, [Fe/H] = +0.44, G9V star CoRoT-33. The orbit is eccentric (e = 0.07) with a period of 5.82 d. The companion, CoRoT-33b, is thus a new member in the so-called brown dwarf desert. The orbital period is within 3% to a 3:2 resonance with the rotational period of the star. CoRoT-33b may be an important test case for tidal evolution studies. The true frequency of brown dwarfs close to their host stars (P < 10 d) is estimated to be approximately 0.2% which is about six times smaller than the frequency of hot Jupiters in the same period range. We suspect that the frequency of brown dwarfs declines faster with decreasing period than that of giant planets.

引用

页数：12

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