HAT-P-65b AND HAT-P-66b: TWO TRANSITING INFLATED HOT JUPITERS AND OBSERVATIONAL EVIDENCE FOR THE REINFLATION OF CLOSE-IN GIANT PLANETS

被引：56

作者：

Hartman, J. D. ^{[1
]}

Bakos, G. A. ^{[1
]}

Bhatti, W. ^{[1
]}

Penev, K. ^{[1
]}

Bieryla, A. ^{[2
]}

Latham, D. W. ^{[2
]}

Kovacs, G. ^{[3
]}

Torres, G. ^{[2
]}

Csubry, Z. ^{[1
]}

de Val-Borro, M. ^{[1
]}

Buchhave, L. ^{[4
]}

Kovacs, T. ^{[3
]}

Quinn, S. ^{[5
]}

Howard, A. W. ^{[6
]}

Isaacson, H. ^{[7
]}

Fulton, B. J. ^{[6
]}

Everett, M. E. ^{[8
]}

Esquerdo, G. ^{[2
]}

Beky, B. ^{[13
]}

Szklenar, T. ^{[9
]}

Falco, E. ^{[2
]}

Santerne, A. ^{[11
]}

Boisse, I. ^{[10
]}

Hebrard, G. ^{[12
]}

Burrows, A. ^{[1
]}

Lazar, J.

Papp, I.

Sari, P.

机构：

[1] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[2] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[3] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary

[4] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark

[5] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA

[6] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[7] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA

[8] Natl Opt Astron Observ, Tucson, AZ 85726 USA

[9] Hungarian Astron Assoc, Budapest, Hungary

[10] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

[11] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, PT-4150762 Oporto, Portugal

[12] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, 98bis Blvd Arago, F-75014 Paris, France

[13] Google, Googleplex, 1600 Amphitheatre Pkwy, Mountain View, CA 94043 USA

来源：

ASTRONOMICAL JOURNAL | 2016年 / 152卷 / 06期

关键词：

stars:; individual; (HAT-P-65; GSC; 1111-00383; HAT-P-66; 3814-00307); techniques:; photometric; techniques: spectroscopic; SOLAR-TYPE STAR; METAL-POOR STAR; BRIGHT F-STAR; RISE LIGHT CURVES; SUN-LIKE STAR; K-DWARF STAR; LOW-DENSITY; EXTRASOLAR PLANET; ECCENTRIC ORBIT; KEPLER FIELD;

D O I：

10.3847/0004-6256/152/6/182

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the discovery of the transiting exoplanets HAT-P-65b and HAT-P-66b, with orbital periods of 2.6055 and 2.9721 days, masses of 0.527 +/- 0.083 M-J and 0.783 +/- 0.057 M-J, and inflated radii of 1.89 +/- 0.13 R-J and 1.59(-0.10)(+0.16) R-J, respectively. They orbit moderately bright (V = 13.145 +/- 0.029 and V = 12.993 +/- 0.052) stars of mass 1.212 +/- 0.050 M-circle dot and 1.255(-0.054)(-0.107) M-circle dot. The stars are at the main-sequence turnoff. While it is well known that the radii of close-in giant planets are correlated with their equilibrium temperatures, whether or not the radii of planets increase in time as their hosts evolve and become more luminous is an open question. Looking at the broader sample of well-characterized close-in transiting giant planets, we find that there is a statistically significant correlation between planetary radii and the fractional ages of their host stars, with a false-alarm probability of only 0.0041%. We find that the correlation between the radii of planets and the fractional ages of their hosts is fully explained by the known correlation between planetary radii and their present-day equilibrium temperatures; however, if the zero-age main-sequence equilibrium temperature is used in place of the present-day equilibrium temperature, then a correlation with age must also be included to explain the planetary radii. This suggests that, after contracting during the pre-main-sequence, close-in giant planets are reinflated over time due to the increasing level of irradiation received from their host stars. Prior theoretical work indicates that such a dynamic response to irradiation requires a significant fraction of the incident energy to be deposited deep within the planetary interiors.

引用

页数：32

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