J/MNRAS/414/418 Chromospheric Mg II h+k flux of evolved stars (Perez+, 2011)
The basal chromospheric Mg II h+k flux of evolved stars: probing the energy
dissipation of giant chromospheres.
Perez Martinez M.I., Schroder K.-P., Cuntz M.
<Mon. Not. R. Astron. Soc., 414, 418-427 (2011)>
=2011MNRAS.414..418P 2011MNRAS.414..418P
ADC_Keywords: Stars, late-type ; Stars, giant ; Stars, supergiant ;
Effective temperatures
Keywords: stars: activity - stars: chromospheres - stars: late-type -
stars: mass-loss - supergiants - stars: winds, outflows
Abstract:
Of a total of 177 cool G, K and M giants and supergiants, we measured
the MgII h+k line emission of extended chromospheres in
high-resolution (LWR) International Ultraviolet Explorer (IUE) spectra
by using the IUE final data archive at the Space Telescope Science
Institute (STScI) and derived the respective stellar surface fluxes.
They represent the chromospheric radiative energy losses presumably
related to basal heating by the dissipation of acoustic waves, plus a
highly variable contribution due to magnetic activity.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 60 177 Physical and empirical surface fluxes of the
chromospheric MgII h+k line emission of 177
cool giants and supergiants from the IUE final
data archive, together with B-V, V, BC and
logTeff (see Section 2)
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See also:
VI/110 : Final Merged Log of IUE Observations (NASA-ESA, 2000)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HD HD number of the star
7- 8 A2 --- n_HD [*+d ] Note (1)
10- 13 F4.2 mag B-V B-V colour index
15- 18 F4.2 mag V-K V-K colour index
20- 27 E8.3 10mW/m2/nm FMg MgII h+k chromospheric emission-line
flux (in erg/cm2/s/Å)
29- 33 F5.2 mag BC.V Bololetric correction in V band
35- 38 F4.2 mag BC.K Bolometric correction in K band
40- 44 F5.3 [K] logTe.B Effective temperature from B-V
46- 50 F5.3 [K] logTe.V Effective temperature from V-K
52- 55 F4.2 [mW/m2] logF.B MgII h+k chromospheric emission-line
surface flux from B-V
57- 60 F4.2 [mW/m2] logF.V MgII h+k chromospheric emission-line
surface flux from V-K
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Note (1): Notes as follows:
* = star with a minimum flux obtained from several observations
+ = star used to determine the basal flux line using the B-V
colour transformation
d = star associated with the V-K colour transformation
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 12-Jan-2012