Chandra HETG X-Ray Spectra and Variability of π Aqr, a γ Cas-type Be Star

被引：2

作者：

Huenemoerder, David P. ^{[1
]}

Pradhan, Pragati ^{[2
]}

Canizares, Claude R. ^{[1
]}

Gunderson, Sean ^{[1
]}

Ignace, Richard ^{[3
]}

Nichols, Joy S. ^{[4
]}

Pollock, A. M. T. ^{[5
]}

Schulz, Norbert S. ^{[1
]}

Swarm, Dustin K. ^{[6
]}

Torrejon, Jose M. ^{[7
]}

机构：

[1] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[2] Embry Riddle Aeronaut Univ, Dept Phys & Astron, 3700 Willow Creek Rd, Prescott, AZ 86301 USA

[3] East Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA

[4] Harvard & Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[5] Univ Sheffield, Dept Phys & Astron, Hounsfield Rd, Sheffield S3 7RH, England

[6] Univ Iowa, Dept Phys & Astron, Iowa City, IA USA

[7] Inst Univ Fis Aplicada Ciencias & Tecnl, Univ Alicante, E-03690 Alicante, Spain

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2024年 / 966卷 / 02期

关键词：

OPTICAL OBSERVATIONS;

D O I：

10.3847/2041-8213/ad4095

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

High-resolution X-ray spectra of pi Aqr, a gamma Cas-type star, obtained with the Chandra/HETG spectrometer, revealed emission lines of H-like ions of Mg, Si, S, and Fe; a strong, hard continuum; and a lack of He-like ions, indicating the presence of very hot thermal plasma. The X-ray light curve showed significant fluctuations, with coherent variability at a period of about 3400 s in one observation. The hardness ratio was relatively constant except for one observation in which the spectrum was much harder and more absorbed. We interpret the X-ray emission as arising from accretion onto the secondary, which is likely a magnetic white dwarf, an intermediate polar system.

引用

页数：6

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