MODELING OF THE HOT JUPITER HAT-P-32 b AND TRANSIT ABSORPTIONS IN EXCITED HYDROGEN AND HELIUM ATOM LINES

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Abstract

The results of absorption modeling in the hydrogen Hα 6563 Å and helium 10830 Å lines for the hot Jupiter HAT-P-32 b are presented. The modeling was performed using a three-dimensional hydrodynamic code together with the Monte Carlo model of Lyα photon transport. A wide range of stellar radiation and atmospheric parameters was considered. It was found that the measured spectrally resolved transit absorption in both lines can be well described by model calculations with the stellar radiation in the XUV range limited to 200 erg/cm2/s per 1 AU, the helium content in the planet's atmosphere He/H=2/98 and metallicity [Fe/H] = -1. It is shown that absorption in the helium line occurs uniformly in a large volume of the outflowing atmosphere, and in the hydrogen line — in a layer of 1.5–2.75 planet radii.

About the authors

S. S. Sharipov

Institute of Laser Physics SB RAS

Email: stas.sharipov@mail.ru
Novosibirsk, Russia

I. F. Shaikhislamov

Institute of Laser Physics SB RAS; Institute of Astronomy of the RAS; Novosibirsk State Technical University

Novosibirsk, Russia; Moscow, Russia; Novosibirsk, Russia

I. B. Miroshnichenko

Institute of Laser Physics SB RAS; Novosibirsk State Technical University

Novosibirsk, Russia; Novosibirsk, Russia

M. S. Rumenskikh

Institute of Laser Physics SB RAS; Institute of Astronomy of the RAS; Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation

Novosibirsk, Russia; Moscow, Russia; Moscow, Russia

A. V. Shepelin

Institute of Laser Physics SB RAS

Novosibirsk, Russia

M. P. Golubovsky

Institute of Laser Physics SB RAS

Novosibirsk, Russia

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