J/A+A/556/A38 Period-mass-loss rate relation of Miras (Uttenthaler, 2013)
Period-mass-loss rate relation of Miras with and without technetium.
Uttenthaler S.
<Astron. Astrophys. 556, A38 (2013)>
=2013A&A...556A..38U 2013A&A...556A..38U
ADC_Keywords: Stars, variable ; Photometry, infrared
Keywords: stars: AGB and post-AGB - stars: late-type - stars: evolution -
stars: mass-loss - stars: oscillations
Abstract:
We report the discovery that Mira variables with and without
absorption lines of the element technetium (Tc) occupy two different
regions in a diagram of near- to mid-IR colour versus pulsation
period. Tc is an indicator of a recent or ongoing mixing event called
the third dredge-up (3DUP), and the near- to mid-IR colour, such as
the (K-[22]) colour where [22] is the the 22um band of the WISE space
observatory, is an indicator of the dust mass-loss rate of a star.
We collected data from the literature about the Tc content, pulsation
period, and near- and mid-IR magnitudes of more than 190 variable
stars on the asymptotic giant branch (AGB) to which Miras belong. The
sample is naturally biased towards optical AGB stars, which have low
to intermediate (dust) mass-loss rates.
Description:
Table 1 is a collection of information on the technetium (Tc) content,
pulsation period, and IR photometry of AGB variables, without claim of
completeness, in particular for the semi-regular variables (SRVs). Up
to three references on the Tc content are given. The pulsation period
is the most up-to-date value possible, for many objects based on an
analysis of AAVSO data with the Period04 program (Lenz & Breger,
2005CoAst.146...53L 2005CoAst.146...53L). The spectral (or chemical) type of the star is
taken from the same literature as the information on Tc. A mean K
magnitude and J-K colour is computed from all available literature, as
listed in Sect. 2 of the paper; they are meant to be as close as
possible to cycle-averaged values, to average out the variability of
the objects. Finally, magnitudes are given in the IRAS 12, 25, and 60
micron bands, Akari 9 and 18 micron bands, and WISE 22 micron bands
are given, where fluxes have been converted to magnitudes given the
zero-magnitude fluxes as given in the Note to Table 1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 106 198 Collected data of sample stars
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See also:
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
II/177 : NIR Photometry of a Sample of IRAS Point Sources (Fouque+ 1992)
II/297 : AKARI/IRC mid-IR all-sky Survey (ISAS/JAXA, 2010)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
J/A+A/317/761 : Miras temperatures, distances + magnitudes (Alvarez+ 1997)
J/A+A/384/925 : Compiled catalog of stellar data of Miras (Kharchenko+ 2002)
J/ApJ/620/961 : Diameters of Mira stars in JHK' bands (Millan-Gabet+, 2005)
J/MNRAS/386/313 : IR observations of Mira variables (Whitelock+, 2008)
J/MNRAS/399/1709 : Near-infrared survey of Miras (Matsunaga+, 2009)
J/ApJS/190/203 : 3.6 years of DIRBE NIR stellar light curves (Price+, 2010)
J/A+A/531/A88 : Optical spectra of 12 Miras (Uttenthaler+, 2011)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Object name
13- 14 I2 --- Tc [0/1] Tc content (0=Tc-poor or 1=Tc-rich)
16- 22 A7 --- Refs Reference(s) of Tc content (1)
25- 29 F5.1 d Per [20.4/926.7]? Period
31- 34 A4 --- Var [Mira SRV] Variability type (2)
36- 37 A2 --- SpT Spectral (chemical) type (3)
39- 44 F6.3 mag Kmag [-4.3/8.1] Mean K-band magnitude computed from
literature (listed in section 2)
46- 50 F5.3 mag J-K Mean J-K colour index
52- 57 F6.3 mag D1.25 ? Mean COBE/DIRBE 1.25mu magnitude, see
Price et al. (2010, Cat. J/ApJS/190/203)
59- 64 F6.3 mag D2.20 ? Mean COBE/DIRBE 2.20mu magnitude, see
Price et al. (2010, Cat. J/ApJS/190/203)
66- 71 F6.3 mag IR12 ? IRAS 12um magnitude
73- 78 F6.3 mag IR25 ? IRAS 25um magnitude
80- 85 F6.3 mag IR60 [-6.1/2.6]? IRAS 60um magnitude
87- 92 F6.3 mag Aka9 ? Akari 9um magnitude
94- 99 F6.3 mag Aka18 ? Akari 18um magnitude
101-106 F6.3 mag WISE22 [-5.9/6.7] WISE 22um magnitude
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Note (1): References as follows:
1 = Little et al., 1987AJ.....94..981L 1987AJ.....94..981L
2 = Smith & Lambert, 1988ApJ...333..219S 1988ApJ...333..219S
3 = Vanture et al., 1991ApJ...381..278V 1991ApJ...381..278V
4 = Lebzelter & Hron, 1999A&A...351..533L 1999A&A...351..533L
5 = van Eck & Jorissen, 1999A&A...345..127V 1999A&A...345..127V
6 = van Eck et al., 2000A&AS..145...51V 2000A&AS..145...51V
7 = Lebzelter & Hron, 2003A&A...411..533L 2003A&A...411..533L
8 = Uttenthaler et al., 2007A&A...463..251U 2007A&A...463..251U
9 = Uttenthaler & Lebzelter, 2010A&A...510A..62U 2010A&A...510A..62U
10 = Uttenthaler et al., 2011A&A...531A..88U 2011A&A...531A..88U, Cat. J/A+A/531/A88
11 = Smolders et al., 2012A&A...540A..72S 2012A&A...540A..72S
12 = Abia et al., 2002ApJ...579..817A 2002ApJ...579..817A
13 = Barnbaum & Morris, 1993AAS...182.4617B 1993AAS...182.4617B
Note (2): Variability type:
Mira = Mira-like variable
SRV = semi-regular variable
Note (3): Spectral (chemical) type:
M = Spectral type M (bands of TiO, VO)
MS = Spectral type MS (bands of TiO, VO, weak ZrO)
S = Spectral type S (strong bands of ZrO, weak TiO)
C = Spectral type C (bands of CN, C2)
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Acknowledgements:
Stefan Uttenthaler, stefan.uttenthaler(at)univie.ac.at
(End) S. Uttenthaler [Dep. Astrophys., U. Vienna], P. Vannier [CDS] 24-Jun-2013