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J/ApJ/797/31   The G+M eclipsing binary V530 Orionis photometry  (Torres+, 2014)

The G+M eclipsing binary V530 Orionis: a stringent test of magnetic stellar evolution models for low-mass stars. Torres G., Lacy C.H.S., Pavlovski K., Feiden G.A., Sabby J.A., Bruntt H., Clausen J.V. <Astrophys. J., 797, 31 (2014)> =2014ApJ...797...31T (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Binaries, eclipsing ; Radial velocities ; Photometry, uvby Keywords: binaries: eclipsing - stars: evolution - stars: fundamental parameters - stars: individual: V530 Ori - techniques: photometric Abstract: We report extensive photometric and spectroscopic observations of the 6.1 day period, G+M-type detached double-lined eclipsing binary V530 Ori, an important new benchmark system for testing stellar evolution models for low-mass stars. We determine accurate masses and radii for the components with errors of 0.7% and 1.3%, as follows: MA=1.0038±0.0066 M, MB=0.5955±0.0022 M, RA=0.980±0.013 R, and RB=0.5873±0.0067 R. The effective temperatures are 5890±100 K (G1 V) and 3880±120 K (M1 V), respectively. A detailed chemical analysis probing more than 20 elements in the primary spectrum shows the system to have a slightly subsolar abundance, with [Fe/H]=-0.12±0.08. A comparison with theory reveals that standard models underpredict the radius and overpredict the temperature of the secondary, as has been found previously for other M dwarfs. On the other hand, models from the Dartmouth series incorporating magnetic fields are able to match the observations of the secondary star at the same age as the primary (∼3 Gyr) with a surface field strength of 2.1±0.4 kG when using a rotational dynamo prescription, or 1.3±0.4 kG with a turbulent dynamo approach, not far from our empirical estimate for this star of 0.83±0.65 kG. The observations are most consistent with magnetic fields playing only a small role in changing the global properties of the primary. The V530 Ori system thus provides an important demonstration that recent advances in modeling appear to be on the right track to explain the long-standing problem of radius inflation and temperature suppression in low-mass stars. Description: V530 Ori was monitored spectroscopically with three different instruments over a period of more than 17 yr. Observations began at the Harvard-Smithsonian Center for Astrophysics (CfA) in 1996 June with a Cassegrain-mounted echelle spectrograph ("Digital Speedometer", DS; Latham 1992ASPC...32..110L) attached to the 1.5 m Tillinghast reflector at the F. L. Whipple Observatory (Mount Hopkins, AZ). We gathered a further 30 spectra of V530 Ori at the Kitt Peak National Observatory (KPNO) from 1999 March to 2001 January, using the coude-feed telescope and the coude spectrometer. Finally, 41 additional observations were obtained at the CfA from 2009 November to 2014 March with the Tillinghast Reflector Echelle Spectrograph (TRES; Furesz 2008, PhD thesis , Univ. Szeged, Hungary) on the 1.5 m telescope mentioned earlier. Two sets of V-band images of V530 Ori were obtained with independent robotic telescopes operating at the University of Arkansas (URSA WebScope) and near Silver City, NM (NFO WebScope) from 2001 January to 2012 February. Differential photometric measurements of V530 Ori were also gathered with the Stromgren Automatic Telescope at ESO (La Silla, Chile), during several campaigns from 2001 January to 2006 February. Objects: ----------------------------------------------------- RA (ICRS) DE Designation(s) ----------------------------------------------------- 06 04 33.8 -03 11 52 V530 Ori = V* V530 Ori ----------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 47 41 Times of eclipse for V530 Ori table2.dat 50 143 Heliocentric radial velocity measurements of V530 Ori table6.dat 24 5137 Differential V-band measurements of V530 Ori from URSA table7.dat 24 3024 Differential V-band measurements of V530 Ori from NFO table8.dat 42 720 Differential uvby measurements of V530 Ori
See also: V/118 : Catalog of eclipsing binaries parameters (Perevozkina+, 1999) J/A+AS/131/395 : Eclipsing binaries light curves models (Claret 1998) J/A+A/487/1081 : uvby photometry of 6 eclipsing binaries (Clausen+, 2008) J/A+A/387/850 : Radial velocities of eclipsing binaries (Imbert, 2002) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 9 F9.4 yr Obs.Y Year of the observation 11- 20 F10.4 d HJD Heliocentric Julian Date (HJD-2400000) 22- 27 F6.4 d sigma ? Timing uncertainty (1) 29- 32 I4 --- Epoch Cycle number (2) 34 I1 --- Ecl [1/2] Eclipse type (3) 36- 41 F6.4 d O-C The (O-C) residuals 43- 44 A2 --- Type Observation type (4) 46- 47 I2 --- Source [1/12] Source (5)
Note (1): As published, or as measured in the case of our own photometric observations. Adopted uncertainties for the photographic, visual, and photoelectric/CCD measurements with no published errors are 0.028, 0.011, and 0.0001 days, respectively. Other errors have been scaled by iterations during the ephemeris fit by factors of 1.8 and 2.9 for the primary and secondary (see text). Note (2): Counted from the reference time of primary eclipse (see text). Note (3): Eclipse type as follows: 1 = primary; 2 = secondary. Note (4): Type as follows: PG = photographic; V = visual; PE = photoelectric or CCD measurement. Note (5): Source as follows: 1 = Strohmeier (1959, VeBam, 5, 3); 2 = Isles (1988, Brit. Astr. Soc. Circ., 67, 11); 3 = Lacy & Fox (1994IBVS.4009....1L); 4 = Lacy et al. (1999IBVS.4737....1L); 5 = This paper; 6 = Lacy (2002AJ....124.1162L); 7 = Lacy (2004IBVS.5577....1L); 8 = Lacy (2007IBVS.5764....1L); 9 = Nagai (2008, Var. Star Bull. (Japan), 46, 5); 10 = Diethelm (2009IBVS.5894....1D); 11 = Lacy (2011IBVS.5972....1L); 12 = Diethelm (2011IBVS.5992....1D).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 10 F10.4 d HJD Heliocentric Julian Date; (HJD-2400000) 12- 17 F6.4 --- Phase Orbital phase 19- 24 F6.2 km/s RVA Primary radial velocity 26- 32 F7.2 km/s RVB Secondary radial velocity 34- 38 F5.2 km/s (O-C)A Primary (O-C) residual 40- 45 F6.2 km/s (O-C)B Secondary (O-C) residual 47- 50 A4 --- Inst Instrument used (1)
Note (1): Instrument as follows: DS = Digital Speedometer; KPNO = Kitt Peak National Observatory coude-feed telescope and the coude spectrometer; TRES = Tillinghast Reflector Echelle Spectrograph.
Byte-by-byte Description of file: table6.dat table7.dat
Bytes Format Units Label Explanations
1- 11 F11.5 d HJD Heliocentric Julian Date (HJD-2400000) 13- 18 F6.4 --- Phase Phase (G1) 20- 24 F5.3 mag DelVmag Differential V band magnitude
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 11 F11.5 d HJD Heliocentric Julian Date (HJD-2400000) 13- 18 F6.4 --- Phase Phase (G1) 20- 24 F5.3 mag Delumag Differential u band magnitude 26- 30 F5.3 mag Delvmag Differential v band magnitude 32- 36 F5.3 mag Delbmag Differential b band magnitude 38- 42 F5.3 mag Delymag Differential y band magnitude
Global notes: Note (G1): Phase counted from the reference epoch of primary eclipse given in Section 2.
History: * 22-Aug-2017 : From electronic version of the journal * 19-Sep-2017 : Corrected table2 with minus signs from author (Guillermo Torres, gtorres(at)cfa.harvard.edu)
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 14-Aug-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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