An upper limit on the reflected light from the planet orbiting the star τ bootis

David Charbonneau; Robert W. Noyes; Sylvain G. Korzennik; Peter Nisenson; Jha Saurabh; Steven S. Vogt; Robert I. Kibrick

doi:10.1086/312234

An upper limit on the reflected light from the planet orbiting the star τ bootis

David Charbonneau, Robert W. Noyes, Sylvain G. Korzennik, Peter Nisenson, Jha Saurabh, Steven S. Vogt, Robert I. Kibrick

Research output: Contribution to journal › Article › peer-review

126 Scopus citations

Abstract

The planet orbiting τ Boo at a separation of 0.046 AU could produce a reflected light flux as bright as 1 x 10^-4 relative to that of the star. A spectrum of the system will contain a reflected light component which varies in amplitude and Doppler shift as the planet orbits the star. Assuming the secondary spectrum is primarily the reflected stellar spectrum, we can limit the relative reflected light flux to be less than 5 x 10^-5. This implies an upper limit of 0.3 for the planetary geometric albedo near 480 nm, assuming a planetary radius of 1.2 R_Jup. This albedo is significantly less than that of any of the giant planets of the solar system and is not consistent with certain published theoretical predictions.

Original language	English (US)
Pages (from-to)	L145-L148
Journal	Astrophysical Journal
Volume	522
Issue number	2 PART 2
DOIs	https://doi.org/10.1086/312234
State	Published - Sep 10 1999
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Planetary systems
Stars: Individual (τ Bootis)
Techniques: Spectroscopic

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10.1086/312234

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title = "An upper limit on the reflected light from the planet orbiting the star τ bootis",

abstract = "The planet orbiting τ Boo at a separation of 0.046 AU could produce a reflected light flux as bright as 1 x 10-4 relative to that of the star. A spectrum of the system will contain a reflected light component which varies in amplitude and Doppler shift as the planet orbits the star. Assuming the secondary spectrum is primarily the reflected stellar spectrum, we can limit the relative reflected light flux to be less than 5 x 10-5. This implies an upper limit of 0.3 for the planetary geometric albedo near 480 nm, assuming a planetary radius of 1.2 RJup. This albedo is significantly less than that of any of the giant planets of the solar system and is not consistent with certain published theoretical predictions.",

keywords = "Planetary systems, Stars: Individual (τ Bootis), Techniques: Spectroscopic",

author = "David Charbonneau and Noyes, {Robert W.} and Korzennik, {Sylvain G.} and Peter Nisenson and Jha Saurabh and Vogt, {Steven S.} and Kibrick, {Robert I.}",

note = "Funding Information: We gratefully acknowledge the NASA/Keck Time Assignment Committee for the observing time allocation. This work was supported in part by NASA grant NAG5-7505.",

year = "1999",

month = sep,

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doi = "10.1086/312234",

language = "English (US)",

volume = "522",

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AU - Charbonneau, David

AU - Noyes, Robert W.

AU - Korzennik, Sylvain G.

AU - Nisenson, Peter

AU - Saurabh, Jha

AU - Vogt, Steven S.

AU - Kibrick, Robert I.

N1 - Funding Information: We gratefully acknowledge the NASA/Keck Time Assignment Committee for the observing time allocation. This work was supported in part by NASA grant NAG5-7505.

PY - 1999/9/10

Y1 - 1999/9/10

N2 - The planet orbiting τ Boo at a separation of 0.046 AU could produce a reflected light flux as bright as 1 x 10-4 relative to that of the star. A spectrum of the system will contain a reflected light component which varies in amplitude and Doppler shift as the planet orbits the star. Assuming the secondary spectrum is primarily the reflected stellar spectrum, we can limit the relative reflected light flux to be less than 5 x 10-5. This implies an upper limit of 0.3 for the planetary geometric albedo near 480 nm, assuming a planetary radius of 1.2 RJup. This albedo is significantly less than that of any of the giant planets of the solar system and is not consistent with certain published theoretical predictions.

AB - The planet orbiting τ Boo at a separation of 0.046 AU could produce a reflected light flux as bright as 1 x 10-4 relative to that of the star. A spectrum of the system will contain a reflected light component which varies in amplitude and Doppler shift as the planet orbits the star. Assuming the secondary spectrum is primarily the reflected stellar spectrum, we can limit the relative reflected light flux to be less than 5 x 10-5. This implies an upper limit of 0.3 for the planetary geometric albedo near 480 nm, assuming a planetary radius of 1.2 RJup. This albedo is significantly less than that of any of the giant planets of the solar system and is not consistent with certain published theoretical predictions.

KW - Planetary systems

KW - Stars: Individual (τ Bootis)

KW - Techniques: Spectroscopic

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An upper limit on the reflected light from the planet orbiting the star τ bootis

Abstract

All Science Journal Classification (ASJC) codes

Keywords

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