ASCA X-ray spectra of the active single stars Beta Ceti and pi(1) Ursae Majoris
1994; IOP Publishing; Volume: 436; Linguagem: Inglês
10.1086/187639
ISSN1538-4357
AutoresS. A. Drake, K. P. Singh, N. E. White, Theodore Simon,
Tópico(s)Astronomy and Astrophysical Research
Resumoview Abstract Citations (60) References (13) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS ASCA X-Ray Spectra of the Active Single Stars beta Ceti and pi 1 Ursae Majoris Drake, S. A. ; Singh, K. P. ; White, N. E. ; Simon, Theodore Abstract We present X-ray spectra obtained by ASCA of two single, active stars, the G dwarf pi(1) UMa, and the G9/K0 giant Beta Cet. The spectra of both stars require the presence of at least two plasma components with different temperatures, 0.3-0.4 keV and approximately 0.7 keV, in order for acceptable fits to be obtained. The spectral resolving power and signal-to-noise ratio of the solid state imaging spectrometer (SIS) spectra allow us to formally constrain the coronal abundances of a number of elements. In Beta Cet, we find Mg to be overabundant, while other elements such as O, Ne, and N are underabundant, relative to the solar photospheric values. From the lower signal-to-noise ratio SIS spectrum of pi(1) UMa, we find evidence for underabundances of O, Ne, and Fe. These results are discussed in the context of the present understanding of elemental abundances in solar and stellar coronae. Publication: The Astrophysical Journal Pub Date: November 1994 DOI: 10.1086/187639 Bibcode: 1994ApJ...436L..87D Keywords: Abundance; Binary Stars; Dwarf Stars; Giant Stars; Stellar Composition; X Ray Spectra; Imaging Spectrometers; Signal To Noise Ratios; Stellar Coronas; Astrophysics full text sources ADS | data products SIMBAD (4) HEASARC (1)
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