J/MNRAS/411/L46 Exoplanet magnetic fields (Vidotto+, 2011)
Prospects for detection of exoplanet magnetic fields through bow-shock
observations during transits.
Vidotto A.A., Jardine M., Helling C.
<Mon. Not. R. Astron. Soc., 411, L46-L50 (2011)>
=2011MNRAS.411L..46V 2011MNRAS.411L..46V
ADC_Keywords: Stars, double and multiple ; Planets ; Magnetic fields
Keywords: planets and satellites: magnetic fields - stars: coronae -
stars: winds, outflows
Abstract:
An asymmetry between the ingress and egress times was observed in the
near-UV light curve of the transit planet WASP-12b. Such asymmetry led
us to suggest that the early ingress in the UV light curve of
WASP-12b, compared to the optical observations, is caused by a shock
around the planet, and that shocks should be a common feature in
transiting systems. Here, we classify all the transiting systems known
to date according to their potential for producing shocks that could
cause observable light curve asymmetries.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 111 92 *Transiting planetary systems known as of
September 2010.
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Note on table1.dat: Planets are ordered in increasing coronal densities of their
host stars, taken as a proxy for the detection of light curves asymmetries.
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Planet Planet name
14- 18 F5.2 Mjup Mpl Planet mass, in M{Jup} unit
20- 23 F4.2 --- Rpl Planet radius, in R{Jup} unit
25- 29 F5.2 d Per Orbital period
31- 35 F5.3 AU Rorb ?=- Orbital semi-major axis
37- 42 F6.1 pc Dist ?=- Heliocentric distance to the system
44- 51 A8 --- SpType Host star MK spectral type
52- 55 F4.2 Msun M* ?=- Host star mass
57- 60 F4.2 Rsun R* ?=- Host star Radius
62- 66 F5.2 km/s vsini ?=- Sky-projected stellar rotation velocity
67 A1 --- n_vsini [a] a: Gandolfi et al. (2010A&A...524A..55G 2010A&A...524A..55G)
69- 72 F4.2 MK Tmax ?=- Maximum temperature required for
shock formation
74- 79 F6.2 [cm-3] lognu ?=- Local density around the planet for the
confined corona
81- 86 F6.2 [cm-3] logns ?=- Local density around the planet considering
the coronal density scales with Omega*
88- 91 F4.1 --- rM(1) ?=- Relative size of the planet magnetosphere
for a planet with Bp=14G and a star with B*=1G
93- 96 F4.1 --- rM(100) ?=- Relative size of the planet magnetosphere
for a planet with Bp=14G and a star with B*=100G
98-101 F4.2 % f ?=- Minimum planetary magnetic field relative
to the stellar one (f=(Bp/B*)min) that is
required to sustain a magnetosphere
103-111 A9 --- OName Other name of the planet
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Aug-2011