Theoretical Transmission Spectra during Extrasolar Giant Planet Transits

  title={Theoretical Transmission Spectra during Extrasolar Giant Planet Transits},
  author={Sara Seager and Dimitar D. Sasselov},
  journal={The Astrophysical Journal},
  pages={916 - 921}
The recent transit observation of HD 209458 b—an extrasolar planet orbiting a Sun-like star—confirmed that it is a gas giant and determined that its orbital inclination is 85°. This inclination makes possible investigations of the planet atmosphere. In this paper we discuss the planet transmission spectra during a transit. The basic tenet of the method is that the planet atmosphere absorption features will be superimposed on the stellar flux as the stellar flux passes through the planet… 

The spectral characteristics of transiting extrasolar planet

The characteristics of the stellar spectral and flux variations intervened by its extrasolar planet provide dynamic and atmospheric information for both bodies. In this report, a transit modelling

Escaping atmospheres of extrasolar planets

These findings mark the first time that helium is detected from the ground and is unambiguously associated with the planet's orbital motion and the high spectral resolution of the observations allows direct tracking of helium's velocity and verifies that it trails the planet along its orbit.

Transmission Spectra as Diagnostics of Extrasolar Giant Planet Atmospheres

Atmospheres of transiting extrasolar giant planets (EGPs) such as HD 209458b must impose features on the spectra of their parent stars during transits; these features contain information about the

Theory of Extrasolar Giant Planet Transits

We present a synthesis of physical effects influencing the observed light curve of an extrasolar giant planet (EGP) transiting its host star. The synthesis includes a treatment of Rayleigh

Infrared Transmission Spectra for Extrasolar Giant Planets

Among the hot Jupiters known to date that transit their parent stars, the two best candidates to be observed with transmission spectroscopy in the mid-infrared (MIR) are HD 189733b and HD 209458b,

Infrared Light Curves and the Detectability of Close-In Extrasolar Giant Planets

We compute theoretical infrared light curves for several known extrasolar planets. We have constructed a set of routines to calculate the orbital parameters for a given planet and integrate over the

Earth’s transmission spectrum from lunar eclipse observations

The optical and near-infrared transmission spectrum of the Earth, obtained during a lunar eclipse, finds some biologically relevant atmospheric features that are weak in the reflection spectrum are much stronger in the transmission spectrum, and indeed stronger than predicted by modelling.

Detection of an Extrasolar Planet Atmosphere

We report high-precision spectrophotometric observations of four planetary transits of HD 209458, in the region of the sodium resonance doublet at 589.3 nm. We find that the photometric dimming

On Constraining a Transiting Exoplanet’s Rotation Rate with Its Transit Spectrum

We investigate the effect of planetary rotation on the transit spectrum of an extrasolar giant planet. During ingress and egress, absorption features arising from the planet's atmosphere are Doppler

Transits of extrasolar planets

In this paper, we consider the physical properties and characteristic features of extrasolar planets and planetary systems, those, for which the passage of low-orbit giant planets across the stellar



Probable detection of starlight reflected from the giant planet orbiting τ Boötis

In the four years following the discovery of a planet orbiting the star 51 Pegasi, about 20 other planets have been detected through their influence on the radial velocities of lines in the stellar

Detection of Planetary Transits Across a Sun-like Star

High-precision, high-cadence photometric measurements of the star HD 209458 are reported, which is known from radial velocity measurements to have a planetary-mass companion in a close orbit and the detailed shape of the transit curve due to both the limb darkening of thestar and the finite size of the planet is clearly evident.

Photometric Light Curves and Polarization of Close-in Extrasolar Giant Planets

The close-in extrasolar giant planets (CEGPs), ≲0.05 AU from their parent stars, may have a large component of optically reflected light. We present theoretical optical photometric light curves and

Giant Planets at Small Orbital Distances

Using Doppler spectroscopy to detect the reflex motion of the nearby star, 51 Pegasi, Mayor & Queloz (1995) claim to have discovered a giant planet in a 0.05 AU, 4.23 day orbit. They estimate its

Extrasolar Giant Planets under Strong Stellar Irradiation

We investigate irradiation of extrasolar giant planets (EGPs) by treating the radiative transfer in detail, so that the flux from the parent star interacts with all relevant depths of the planetary

On the search for O 2 in extrasolar planets

The present work is a first attempt to investigate the feasibility of the optical detection of absorption lines in the atmosphere of extrasolar planets. Two cases are considered: (1) the “reflection”

The Spectroscopic Orbit of the Planetary Companion Transiting HD 209458

A spectroscopic orbit with period P=3.52433+/-0.00027 days for the planetary companion that transits the solar-type star HD 209458 is reported, based on a new analysis of the iron lines in the HIRES template spectrum and also on the absolute magnitude, effective temperature, and color of the star.

An Upper Limit on the Reflected Light from the Planet Orbiting the Star τ Bootis

The planet orbiting τ Boo at a separation of 0.046 AU could produce a reflected light flux as bright as 1 × 10-4 relative to that of the star. A spectrum of the system will contain a reflected light

A Transiting “51 Peg-like” Planet

Doppler measurements from Keck exhibit a sinusoidal periodicity in the velocities of the G0 dwarf HD 209458, having a semiamplitude of 81 m s-1 and a period of 3.5239 days, which is indicative of a

Albedo and Reflection Spectra of Extrasolar Giant Planets

We generate theoretical albedo and reflection spectra for a full range of extrasolar giant planet (EGP) models, from Jovian to 51 Pegasi class objects. Our albedo modeling utilizes the latest atomic