J/A+A/663/A115  Contact binary variables X-ray emission within 1kpc (Liu+, 2022)

The X-ray emission of contact binary variables within 1kpc. Lui J., Wu J., Esamdin A., Gu W.-M., Sun M., Wang J. <Astron. Astrophys. 663, A115 (2022)> =2022A&A...663A.115L 2022A&A...663A.115L (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, X-ray ; Binaries, eclipsing ; Stars, variable ; Stars, distances ; Effective temperatures ; Optical Keywords: binaries: close - binaries: eclipsing - stars: variables: general - X-ray: binaries Abstract: The X-ray emission of contact binaries (EW-type) is an important facet of such systems. Thus, X-ray emitting EW-type binaries (EWXs) are ideal laboratories for studying the X-ray radiation saturation mechanisms as well as binary evolution. By assembling the largest sample to date of EWXs with periods of less than 1 day from the All-Sky Automated Survey for Supernovae Variable Stars Database and X-ray catalogs from the XMM-Newton and ROSAT missions, we aim to conduct a systematic population study of X-ray emission properties of EWXs within 1 kpc. We carried out correlation analyses for the X-ray luminosity, logLX, and X-ray activity level log(LX/Lbol) versus the orbital period, P, effective temperature, Teff, metallicity [Fe/H], and the surface gravity logg of EWXs. We investigated the relation between X-ray emission and the mass of component stars in the binary systems. We also performed sample simulations to explore the degeneracy between period, mass, and effective temperature for EWXs. We find strong P-logLX and P-log(LX/Lbol) correlations for EWXs with P≤0.44-days and we provide the linear parametrizations for these relations, on the basis of which the orbital period can be treated as a good predictor for log-LX and log(LX/Lbol). The aforementioned binary stellar parameters are all correlated with log-LX, while only Teff exhibits a strong correlation with log(LX/Lbol). Then, EWXs with higher temperature show lower X-ray activity level, which could indicate the thinning of the convective area related to the magnetic dynamo mechanism. The total X-ray luminosity of an EWX is essentially consistent with that of an X-ray saturated main sequence star with the same mass as its primary, which may imply that the primary star dominates the X-ray emission. The monotonically decreasing P-log(LX/Lbol) relation and the short orbital periods indicate that EWXs could all be in the X-ray saturated state, and they may inherit the changing trend of the saturated X-ray luminosities along with the mass shown by single stars. For EWXs, the orbital period, mass, and effective temperature increase in concordance. We demonstrate that the period P=0.44-days corresponds to the primary mass of ∼1.1M, beyond which the saturated X-ray luminosity of single stars will not continue to increase with mass. This explains the break in the positive P-logLX relation for EWXs with P>0.44-days. Description: Parameters of 376 and 319 for EWXs date from the All-Sky Automated Survey for Supernovae Variable Stars Database and X-ray catalogs from the XMM-Newton (STW sample) and ROSAT missions (SRASS sample). Several parameters of 139 EWXs with spectra from LAMOST DR7 (Spec-EWX sample). Several parameters of 12279 X-ray luminosity upper limits from XMM-Newton pointed and slew surveys for EW-type binaries. Several parameters of 13769 X-ray luminosity upper limits from ROSAT survey for EW-type binaries. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 142 376 Properties of EWXs in STW (Groups A, B and C) table2.dat 69 319 Properties of objects in SRASS table3.dat 72 139 Several parameters of EWXs in Spec-EWX sample table4.dat 54 12279 Several parameters of X-ray luminosity upper limits from XMM-Newton pointed and slew surveys for EW-type binaries table5.dat 54 13769 Several parameters of X-ray luminosity upper limits from ROSAT survey for EW-type binaries -------------------------------------------------------------------------------- See also: II/366 : ASAS-SN catalog of variable stars (Jayasinghe+, 2018-2020) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 A1 --- Group [ABC] Group 3- 30 A28 --- ASAS-SN ASAS-SN identifier (JHHMMSS.ss+DDMMSS.s) 32- 40 F9.5 deg RAdeg Right Ascension (J2000) 42- 50 F9.5 deg DEdeg Declination (J2000) 52- 58 F7.5 d Per The interval of time between the recurrence of phases in a periodic phenomenon 60- 65 F6.4 mas Plx Gaia DR2 parallax 67- 72 F6.2 pc Dist Linear distance 74- 94 A21 --- 4XMM-DR9 Unique source name in 4XMM-DR9 catalog 96-101 F6.3 [10-7W] logLX X-ray Luminosity in 0.2-12keV band 103-112 A10 --- ATLASType Final ATLAS variable classification 114-120 A7 --- WISEType Final WISE variable classification 122-127 F6.3 mag AG ? Line-of-sight extinction in the G band 128 A1 --- n_AG [*] * for AG fixed to 0.600 (see Section 3.1 for details) 130-135 F6.3 [10-7W] logLbol ? Bolometric luminosity 137-142 F6.3 --- log(LX/Lbol) ? Ratio of X-ray luminosity to bolometric luminosity -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 9 F9.5 deg RAdeg Right ascension (J2000) 11- 19 F9.5 deg DEdeg Declination (J2000) 21- 27 F7.5 d Per The interval of time between the recurrence of phases in a periodic phenomenon 29- 34 F6.2 pc Dist Linear distance 36- 41 F6.3 [10-7W] logLX X-ray Luminosity in 0.2-12keV band 43- 47 F5.3 mag AG ? Line-of-sight extinction in the G band 48 A1 --- n_AG [*] * for AG fixed to 0.600 (see Section 3.1 for details) 50- 56 F7.3 [10-7W] logLbol ? Bolometric luminosity 58- 63 F6.3 --- log(LX/Lbol) ? Ratio of X-ray luminosity to bolometric luminosity 65- 69 A5 --- Ref Reference (1) -------------------------------------------------------------------------------- Note (1): References as follows: 1 = Stepien et al. (2001A&A...370..157S 2001A&A...370..157S) 2 = Geske et al. (2006AJ....131..633G 2006AJ....131..633G, Cat. J/AJ/131/633) 3 = Chen et al. (2006AJ....131..990C 2006AJ....131..990C) 4 = Duplication in STW 5 = This Work -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 9 F9.5 deg RAdeg Right ascension (J2000) 11- 19 F9.5 deg DEdeg Declination (J2000) 21- 26 F6.3 [10-7W] logLX X-ray Luminosity in 0.2-12keV band 28- 34 F7.5 d Per The interval of time between the recurrence of phases in a periodic phenomenon 36- 42 F7.2 K Teff Effective temperature from LAMOST DR7 44- 49 F6.2 K e_Teff The error of effective temperature from LAMOST DR7 51- 56 F6.3 [-] [Fe/H] Metallicity from LAMOST DR7 58- 61 F4.2 [-] e_[Fe/H] The error of metallicity from LAMOST DR7 63- 67 F5.3 [cm/s2] logg The log surface gravity from LAMOST DR7 69- 72 F4.2 [cm/s2] e_logg The error of log surface gravity from LAMOST DR7 -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 9 F9.5 deg RAdeg Right ascension (J2000) 11- 19 F9.5 deg DEdeg Declination (J2000) 21- 31 A11 --- Modes Missions operate in survey, slew and/or pointed observation mode 33- 39 F7.5 d Per The interval of time between the recurrence of phases in a periodic phenomenon 41- 46 F6.2 pc Dist Linear distance 48 A1 --- l_logLX Limit flag on logLX 49- 54 F6.3 [10-7W] logLX Upper limits of X-ray luminosity in 0.2-12keV band -------------------------------------------------------------------------------- Acknowledgements: Junhui Liu, wujianfeng(at)xmu.edu.cn
(End) Junhui Liu [Xiamen, Fujian, China], Patricia Vannier [CDS] 18-May-2022
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