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Garcia, M., Baliunas, S.L., Conroy, M., Johnston, M.D., Ralph, E., Roberts, W., Schwartz, D.A. and Tonry, J. (1980) Optical Identification of H0123+075 and 4u 1137-65: Hard X-Ray Emission from Rs Canum Venaticorum Systems. The Astrophysical Journal, 240, L107-L110.
https://doi.org/10.1086/183334

has been cited by the following article:

• TITLE: The 6.7 keV Line Emission from the Stellar Flare of Algol

  AUTHORS: Ambrose C. Eze, Sudum Esaenwi, Abraham I. Chima

  KEYWORDS: Flare Stars, Active Eclipsing Binary, Algol, Corona, Stellar Flare, X-Ray, Line Emission

  JOURNAL NAME: Journal of High Energy Physics, Gravitation and Cosmology, Vol.5 No.4, September 18, 2019

  ABSTRACT: We present spectral analysis of Algol stellar flare data. The 2-day observation of Algol in our Galaxy was done by Suzaku Satellite. Algol binary system consists of two component stars that eclipse one another periodically. The stellar magnetic field activities and Roche Lobe overflow/mass transfer mechanisms during rapid rotation of the component stars generate an X-ray emission. The variation in brightness of the stellar flare from epoch to epoch provides useful information of stellar properties of the component stars. The atomic physics of the Kα line emission process in the vicinities of chromospherically active and X-ray flare stars, and binaries is well understood. The photo ionization/collisional excitation in the Algol’s corona produces 6.7 keV line emission. The accumulated spectra in X-ray Imaging Spectrometer (XIS) sensors fitted combined with bremsstrahlung model and Gaussian line show a strong fixed X-ray energy of 6.7 keV.