2011A&A...532A...1S


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.26CET20:31:16

2011A&A...532A...1S - Astronomy and Astrophysics, volume 532A, 1-1 (2011/8-1)

Thermal phase curves of nontransiting terrestrial exoplanets. I. Characterizing atmospheres.

SELSIS F., WORDSWORTH R.D. and FORGET F.

Abstract (from CDS):

Although transit spectroscopy is a very powerful method for studying the composition, thermal properties, and dynamics of exoplanet atmospheres, only a few transiting terrestrial exoplanets will be close enough to allow significant transit spectroscopy with the current and forthcoming generations of instruments. Thermal phase curves (variations in the apparent infrared emission of the planet with its orbital phase) have been observed for hot Jupiters in both transiting and nontransiting configurations, and have been used to put constraints on the temperature distribution and atmospheric circulation. This method could be applied to hot terrestrial exoplanets. We study the wavelength and phase changes of the thermal emission of a tidally-locked terrestrial planet as atmospheric pressure increases. We address the observability of these multiband phase curves and the ability to use them to detect atmospheric constituents. We used a 3D climate model (GCM) to simulate the CO2 atmosphere of a terrestrial planet on an 8-day orbit around an M 3 dwarf and its apparent infrared emission as a function of its orbital phase. We estimated the signal to photon-noise ratio in narrow bands between 2.5 and 20µm for a 10pc target observed with a 6m and a 1.5m telescope (respectively the sizes of JWST and EChO). Atmospheric absorption bands produce associated signatures in what we call the variation spectrum. Atmospheric windows probing the near surface atmospheric layers are needed to produce large, observable phase-curve amplitudes. The number and transparency of these windows, hence the observability of the phase curves and the molecular signatures, decreases with increasing pressure. Planets with no atmosphere produce large variations and can be easily distinguished from dense absorbing atmospheres. Photon-noise limited spectro-photometry of nearby systems could allow us to detect and characterize the atmosphere of nontransiting terrestrial planets known from radial velocity surveys. Two obvious impediments to these types of observations are the required photometric sensitivity (10–5) over the duration of at least one orbit (8-days in the studied case) and the intrinsic stellar variability. However, overcoming these obstacles would give access to one order of magnitude more targets than does transit spectroscopy.

Abstract Copyright:

Journal keyword(s): planets and satellites: atmospheres - planetary systems - standards

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 285968b Pl 04 42 55.7753203198 +18 57 29.394344631           ~ 34 1
2 HD 40307b Pl 05 54 04.2409953924 -60 01 24.491747849           ~ 43 1
3 CoRoT-7b Pl 06 43 49.4690410679 -01 03 46.825797768           ~ 363 1
4 * rho01 Cnc e Pl 08 52 35.8113282132 +28 19 50.956901366           ~ 424 1
5 BD+20 2465 Er* 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   dM3 1170 0
6 * 61 Vir b Pl 13 18 24.3142756 -18 18 40.304648           ~ 38 1
7 BD-07 4003e Pl 15 19 26.8271336166 -07 43 20.190958776           ~ 66 1
8 BD-07 4003d Pl 15 19 26.8271336166 -07 43 20.190958776           ~ 139 1
9 BD-07 4003b Pl 15 19 26.8271336166 -07 43 20.190958776           ~ 73 1
10 BD-07 4003 BY* 15 19 26.8271336166 -07 43 20.190958776 13.403 11.76 10.560 9.461 8.911 M3V 549 2
11 NAME G 139-21b Pl 17 15 18.9337265994 +04 57 50.064695682           ~ 562 1
12 CD-46 11540b Pl 17 28 39.9455601300 -46 53 42.693246243           ~ 43 1
13 Kepler-10b Pl 19 02 43.0612302512 +50 14 28.700759378           ~ 254 1
14 BD-15 6290 BY* 22 53 16.7323107416 -14 15 49.303409936 12.928 11.749 10.192 9.013 7.462 M3.5V 874 1
15 BD-15 6290d Pl 22 53 16.7323107416 -14 15 49.303409936           ~ 135 1

    Equat.    Gal    SGal    Ecl

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