The Eclipsing Binary System AR Monocerotis

Williamon, R. M.; Hamme, W. Van; Torres, Guillermo; Sowell, James R.; Ponce, V.

doi:10.1086/430215

Cited by 15 publications

(9 citation statements)

References 23 publications

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“…For example, we note that the mass of the cooler star in AV Del is quite similar to that of the mass-losing secondaries in all the other cool Algol systems for which estimates are available (RZ Cnc, AR Mon, RT Lac, AD Cap, RV Lib, BD +05 706, and V756 Sco;Popper 1976Popper , 1991Popper , 1996Torres et al 2003;Williamon et al 2005). These components are all around $0.45 to $0.75 M and are presumably in the process of being stripped to their helium cores.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 66%

“…Only six of the members have spectroscopic orbits for both components (RZ Cnc, AR Mon, RT Lac, AD Cap, RV Lib, and BD +05 706;Popper 1976Popper , 1991Torres et al 1998;Williamon et al 2005). All of these systems, with the exception of RV Lib, have had light-curve analyses performed on them that have yielded the absolute masses and radii necessary in order to understand their properties.…”

Section: Introductionmentioning

confidence: 99%

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Optical Photometry and Spectroscopy of the Suspected "Cool Algol" AV Delphini: Determination of the Physical Properties

et al. 2005

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We present new spectroscopic and BVRI photometric observations of the double-lined eclipsing binary AV Del ( period ¼ 3:85 days) conducted over six observing seasons. A detailed radial velocity and light-curve analysis of the optical data shows the system to be most likely semidetached, with the less massive and cooler star filling its Roche lobe. The system is probably a member of the rare class of ''cool Algol'' systems, which are distinguished from the ''classical'' Algol systems in that the mass-gaining component is also a late-type star rather than a B-or A-type star. By combining the spectroscopic and photometric analyses, we derive accurate absolute masses for the components of M 1 ¼ 1:453 AE 0:028 M and M 2 ¼ 0:705 AE 0:014 M and radii of R 1 ¼ 2:632 AE 0:030 R and R 2 ¼ 4:233 AE 0:060 R , as well as effective temperatures of 6000 AE 200 and 4275 AE 150 K for the primary and secondary, respectively. There are no obvious signs of activity (spottedness) in the optical light curve of the binary.

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Section: Discussion and Concluding Remarksmentioning

confidence: 66%

Section: Introductionmentioning

confidence: 99%

Optical Photometry and Spectroscopy of the Suspected "Cool Algol" AV Delphini: Determination of the Physical Properties

et al. 2005

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“…In all panels, the NICER and MAXI data are shown by triangles and circles, respectively. McDowell et al 1994;Voges et al 1999;Kovári et al 2001;Williamon et al 2005). Each L X is taken from the ROSAT bright source catalog (Voges et al 1999) in order to unify the X-ray band with that used in Wright et al (2011), 0.1-2.4 keV.…”

Section: Coronal Magnetic Activitymentioning

confidence: 99%

The RS CVn–type Star GT Mus Shows Most Energetic X-Ray Flares Throughout the 2010s

Sasaki

Tsuboi

Iwakiri

et al. 2021

ApJ

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We report that the RS CVn-type star GT Mus (HR 4492, HD 101379+HD 101380) was the most active star in the X-ray sky in the last decade in terms of the scale of recurrent energetic flares. We detected 11 flares from GT Mus in 8 yr of observations with the Monitor of All-sky X-ray Image (MAXI) from 2009 August to 2017 August. The detected flare peak luminosities were 1-4 × 10 33 erg s −1 in the 2.0-20.0 keV band for its distance of 109.6 pc. Our timing analysis showed long durations (τ r + τ d ) of 2-6 days with long decay times (τ d ) of 1-4 days. The released energies during the decay phases of the flares in the 0.1-100 keV band were in the range of 1-11 × 10 38 erg, which are at the upper end of the observed stellar flare. The released energies during the whole duration were in the range of 2-13 × 10 38 erg in the same band. We carried out X-ray follow-up observations for one of the 11 flares with the Neutron star Interior Composition Explorer (NICER) on 2017 July 18 and found that the flare cooled quasi-statically. On the basis of a quasi-static cooling model, the flare loop length is derived to be 4 × 10 12 cm (or 60 R ☉ ). The electron density is derived to be 1 × 10 10 cm −3 , which is consistent with the typical value of solar and stellar flares (10 10-13 cm −3 ). The ratio of the cooling timescales between radiative (τ rad ) and conductive (τ cond ) cooling is estimated to be τ rad ∼ 0.1 τ cond from the temperature; thus, radiative cooling was dominant in this flare.

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“…These parameters are now based on whole light and velocity curves, not just on times of minima. Examples of this method, including checks against ephemeris parameters based on eclipse timings, can be found in Van Hamme et al (2001) for CN And and in Williamon et al (2005) for AR Mon.…”

Section: Ephemeris Parametersmentioning

confidence: 99%

HD 71636, A Newly Discovered Eclipsing Binary

Henry¹,

Fekel²,

Sowell³

et al. 2006

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Our differential BV photometric observations, acquired with an automated telescope at Fairborn Observatory, show that HD 71636 is an eclipsing binary. From follow-up red-wavelength spectroscopic observations we classify the primary and secondary as an F2 dwarf and an F5 dwarf, respectively. The system has a period of 5.01329 days and a circular orbit. We used the Wilson-Devinney program to simultaneously solve our BV light curves and radial velocities and determined a number of fundamental properties of the system. Comparison with evolutionary tracks indicates that both stars are well ensconced on the main sequence. The age of the system is about 1.2 billion years.

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The Eclipsing Binary System AR Monocerotis

Cited by 15 publications

References 23 publications

Optical Photometry and Spectroscopy of the Suspected "Cool Algol" AV Delphini: Determination of the Physical Properties

Optical Photometry and Spectroscopy of the Suspected "Cool Algol" AV Delphini: Determination of the Physical Properties

The RS CVn–type Star GT Mus Shows Most Energetic X-Ray Flares Throughout the 2010s

HD 71636, A Newly Discovered Eclipsing Binary

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