HD 147506b: A supermassive planet in an eccentric orbit transiting a bright star

G. Á Bakos; G. Kovács; G. Torres; D. A. Fischer; D. W. Latham; R. W. Noyes; D. D. Sasselov; T. Mazeh; A. Shporer; R. P. Butler; R. P. Stefanik; J. M. Fernández; A. Sozzetti; A. Pal; J. Johnson; G. W. Marcy; J. N. Winn; B. Sipöcz; J. Lázár; I. Papp; P. Sári

doi:10.1086/521866

HD 147506b: A supermassive planet in an eccentric orbit transiting a bright star

G. Á Bakos, G. Kovács, G. Torres, D. A. Fischer, D. W. Latham, R. W. Noyes, D. D. Sasselov, T. Mazeh, A. Shporer, R. P. Butler, R. P. Stefanik, J. M. Fernández, A. Sozzetti, A. Pal, J. Johnson, G. W. Marcy, J. N. Winn, B. Sipöcz, J. Lázár, I. PappP. Sári

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Abstract

We report the discovery of a massive (M_p, = 9.04 ±0.50 M_J) planet transiting the bright (V = 8.7) F8 star HD 147506, with an orbital period of 5.63341 ±0.00013 days and an eccentricity of e = 0.520 ±0.010. From the transit light curve we determine that the radius of the planet is R_p = 0.982_-0.105^+0.038 R _J. HD 147506b (also coined HAT-P-2b) has a mass about 9 times the average mass of previously known transiting exoplanets and a density of ρ_ρ ≈12 g cm^-3, greater than that of rocky planets like the Earth. Its mass and radius are marginally consistent with theories of structure of massive giant planets composed of pure H and He, and accounting for them may require a large (≳100 M_⊕) core. The high eccentricity causes a ninefold variation of insolation of the planet between peri- and apastron. Using follow-up photometry, we find that the center of transit is T_mid = 2,454,212.8559 ± 0.0007 ( HJD) and the transit duration is 0.177 ± 0.002 days.

Original language	English (US)
Pages (from-to)	826-832
Number of pages	7
Journal	Astrophysical Journal
Volume	670
Issue number	1
DOIs	https://doi.org/10.1086/521866
State	Published - Nov 20 2007
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Planetary systems
Stars: individual (HD 147506)

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10.1086/521866

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Bakos, G. Á., Kovács, G., Torres, G., Fischer, D. A., Latham, D. W., Noyes, R. W., Sasselov, D. D., Mazeh, T., Shporer, A., Butler, R. P., Stefanik, R. P., Fernández, J. M., Sozzetti, A., Pal, A., Johnson, J., Marcy, G. W., Winn, J. N., Sipöcz, B., Lázár, J., ... Sári, P. (2007). HD 147506b: A supermassive planet in an eccentric orbit transiting a bright star. Astrophysical Journal, 670(1), 826-832. https://doi.org/10.1086/521866

@article{21557b86a0f34ce4a661afa4b037b377,

title = "HD 147506b: A supermassive planet in an eccentric orbit transiting a bright star",

abstract = "We report the discovery of a massive (Mp, = 9.04 ±0.50 MJ) planet transiting the bright (V = 8.7) F8 star HD 147506, with an orbital period of 5.63341 ±0.00013 days and an eccentricity of e = 0.520 ±0.010. From the transit light curve we determine that the radius of the planet is Rp = 0.982-0.105+0.038 R J. HD 147506b (also coined HAT-P-2b) has a mass about 9 times the average mass of previously known transiting exoplanets and a density of ρρ ≈12 g cm-3, greater than that of rocky planets like the Earth. Its mass and radius are marginally consistent with theories of structure of massive giant planets composed of pure H and He, and accounting for them may require a large (≳100 M⊕) core. The high eccentricity causes a ninefold variation of insolation of the planet between peri- and apastron. Using follow-up photometry, we find that the center of transit is Tmid = 2,454,212.8559 ± 0.0007 ( HJD) and the transit duration is 0.177 ± 0.002 days.",

keywords = "Planetary systems, Stars: individual (HD 147506)",

author = "Bakos, {G. {\'A}} and G. Kov{\'a}cs and G. Torres and Fischer, {D. A.} and Latham, {D. W.} and Noyes, {R. W.} and Sasselov, {D. D.} and T. Mazeh and A. Shporer and Butler, {R. P.} and Stefanik, {R. P.} and Fern{\'a}ndez, {J. M.} and A. Sozzetti and A. Pal and J. Johnson and Marcy, {G. W.} and Winn, {J. N.} and B. Sip{\"o}cz and J. L{\'a}z{\'a}r and I. Papp and P. S{\'a}ri",

year = "2007",

month = nov,

day = "20",

doi = "10.1086/521866",

language = "English (US)",

volume = "670",

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journal = "Astrophysical Journal",

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Bakos, GÁ, Kovács, G, Torres, G, Fischer, DA, Latham, DW, Noyes, RW, Sasselov, DD, Mazeh, T, Shporer, A, Butler, RP, Stefanik, RP, Fernández, JM, Sozzetti, A, Pal, A, Johnson, J, Marcy, GW, Winn, JN, Sipöcz, B, Lázár, J, Papp, I & Sári, P 2007, 'HD 147506b: A supermassive planet in an eccentric orbit transiting a bright star', Astrophysical Journal, vol. 670, no. 1, pp. 826-832. https://doi.org/10.1086/521866

TY - JOUR

T1 - HD 147506b

T2 - A supermassive planet in an eccentric orbit transiting a bright star

AU - Bakos, G. Á

AU - Kovács, G.

AU - Torres, G.

AU - Fischer, D. A.

AU - Latham, D. W.

AU - Noyes, R. W.

AU - Sasselov, D. D.

AU - Mazeh, T.

AU - Shporer, A.

AU - Butler, R. P.

AU - Stefanik, R. P.

AU - Fernández, J. M.

AU - Sozzetti, A.

AU - Pal, A.

AU - Johnson, J.

AU - Marcy, G. W.

AU - Winn, J. N.

AU - Sipöcz, B.

AU - Lázár, J.

AU - Papp, I.

AU - Sári, P.

PY - 2007/11/20

Y1 - 2007/11/20

N2 - We report the discovery of a massive (Mp, = 9.04 ±0.50 MJ) planet transiting the bright (V = 8.7) F8 star HD 147506, with an orbital period of 5.63341 ±0.00013 days and an eccentricity of e = 0.520 ±0.010. From the transit light curve we determine that the radius of the planet is Rp = 0.982-0.105+0.038 R J. HD 147506b (also coined HAT-P-2b) has a mass about 9 times the average mass of previously known transiting exoplanets and a density of ρρ ≈12 g cm-3, greater than that of rocky planets like the Earth. Its mass and radius are marginally consistent with theories of structure of massive giant planets composed of pure H and He, and accounting for them may require a large (≳100 M⊕) core. The high eccentricity causes a ninefold variation of insolation of the planet between peri- and apastron. Using follow-up photometry, we find that the center of transit is Tmid = 2,454,212.8559 ± 0.0007 ( HJD) and the transit duration is 0.177 ± 0.002 days.

AB - We report the discovery of a massive (Mp, = 9.04 ±0.50 MJ) planet transiting the bright (V = 8.7) F8 star HD 147506, with an orbital period of 5.63341 ±0.00013 days and an eccentricity of e = 0.520 ±0.010. From the transit light curve we determine that the radius of the planet is Rp = 0.982-0.105+0.038 R J. HD 147506b (also coined HAT-P-2b) has a mass about 9 times the average mass of previously known transiting exoplanets and a density of ρρ ≈12 g cm-3, greater than that of rocky planets like the Earth. Its mass and radius are marginally consistent with theories of structure of massive giant planets composed of pure H and He, and accounting for them may require a large (≳100 M⊕) core. The high eccentricity causes a ninefold variation of insolation of the planet between peri- and apastron. Using follow-up photometry, we find that the center of transit is Tmid = 2,454,212.8559 ± 0.0007 ( HJD) and the transit duration is 0.177 ± 0.002 days.

KW - Planetary systems

KW - Stars: individual (HD 147506)

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U2 - 10.1086/521866

DO - 10.1086/521866

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VL - 670

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EP - 832

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

ER -

HD 147506b: A supermassive planet in an eccentric orbit transiting a bright star

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