J/A+A/552/A119 Planet-star and moon-planet interaction (Saur+, 2013)
Magnetic energy fluxes in sub-Alfvenic planet star and moon planet interactions.
Saur J., Grambusch T., Duling S., Neubauer F.M., Simon S.
<Astron. Astrophys. 552, A119 (2013)>
=2013A&A...552A.119S 2013A&A...552A.119S
ADC_Keywords: Stars, double and multiple ; Planets ; Magnetic fields
Keywords: planet-star interactions - planets and satellites: general -
planets and satellites: magnetic fields
Abstract:
Electromagnetic coupling of planetary moons with their host planets is
well observed in our solar system. Similar couplings of extrasolar
planets with their central stars have been studied observationally on
an individual as well as on a statistical basis.
We aim to model and to better understand the energetics of planet star
and moon planet interactions on an individual and as well as on a
statistical basis.
Description:
We list stellar wind properties calculated for all extrasolar planets
known until 2012/11/14. Furthermore we provide values of the Poynting
flux and its properties generated at these extrasolar planets. Note,
in many cases stellar properties are unknown and had to be estimated.
Similarly, the existences, strengths and orientations of the magnetic
moments of extrasolar planets are unknown. We used a scaling law to
derive magnetic moments which enter into our calculations of the total
Poynting fluxes. See Section 4.1 of the paper for further details.
Notes:
* All values are local properties at the distance of the exoplanets orbit.
* We use a counterclockwise polar coordinate system.
* Vsw and Br are defined in radial direction, Vorbit and Bphi in
azimuthal direction.
* Vorbit is calculated with Kepler's third law.
* To calculate the relative plasma velocity in the rest-frame of the
extrasolar planets the negative orbital velocity v_orbit must be
considered.
* The model of Parker (1958ApJ...128..664P 1958ApJ...128..664P) was used to calculate
the other stellar wind properties.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 104 850 Stellar wind properties
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See also:
http://exoplanet.eu/catalog : Exoplanet.eu catalog
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Name Name of the extrasolar planet (1)
22- 30 E9.3 AU rexo Distance of planet from its host star
32- 40 E9.3 m/s Vorb Kepler-orbit velocity of the extrasolar planet
42- 50 E9.3 m/s Vsw Stellar wind plasma velocity (2)
52- 60 E9.3 T Br Radial component of stellar wind
magnetic field (3)
62- 71 E10.3 T Bphi Azimuthal component of stellar wind
magnetic field (4)
73- 81 E9.3 kg/m3 rho Stellar wind mass density near planet
83- 91 E9.3 --- MA Alfven Mach number at exoplanet
93-102 E10.3 W Stot Total Poynting flux (5)
104 I1 --- Prop Properties code (6)
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Note (1): Name of the extrasolar planet as listed on http://exoplanet.eu.
For simple I/O we replaced blanks with underscores ('_').
Note (2): Stellar wind plasma velocity directed radially away
from the star near extrasolar planet.
Note (3): Radial component of the stellar wind magnetic field near
extrasolar planet.
Note (4): Azimuthal component of the stellar wind magnetic field near
extrasolar planet.
Note (5): Total Poynting flux in the cA- Alfven wing generated near
extrasolar planet.
Note (6): The properties are number coded as follows:
0 = [MA>1] Alfven Mach number MA is larger 1, thus the
plasma interaction is super-Alfvenic.
1 = [MA<1] cA- wing is connected with the host star.
Exact solution in (53) of the paper was used to
calculate the Poynting flux.
2 = [MA<1] cA- wing is connected with the host star.
Exact solution in (53) of the paper could not be used
to calculate the Poynting flux. We lowered the interaction
strength {bar}alpha to derive a lower limit for the Poynting flux.
3 = [MA<1] cA- wing is not connected with the host star,
both wings point away from the star.
Exact solution in (53) of the paper was used to
calculate the Poynting flux.
4 = [MA<1] cA- wing is not connected with the host star,
both wings point away from the star.
Exact solution in (53) of the paper could not be used to
calculate the Poynting flux. We lowered the interaction
strength {bar}alpha to derive a lower limit for the Poynting flux.
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Acknowledgements:
Joachim Saur, jsaur(at)uni-koeln.de
(End) Patricia Vannier [CDS] 24-Jan-2013