Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations

被引：4

作者：

Vermette, Benjamin ^{[1
]}

Salcedo, Ciro ^{[1
]}

Mori, Kaya ^{[1
]}

Gerber, Julian ^{[1
]}

Yoon, Kyung Duk ^{[1
]}

Bridges, Gabriel ^{[1
]}

Hailey, Charles J. ^{[1
]}

Haberl, Frank ^{[2
]}

Hong, Jaesub ^{[3
]}

Grindlay, Jonathan ^{[3
]}

Ponti, Gabriele ^{[4
]}

Ramsay, Gavin ^{[5
]}

机构：

[1] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[2] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany

[3] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[4] INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy

[5] Armagh Observ & Planetarium, Coll Hill, Armagh BT61 9DG, North Ireland

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 954卷 / 02期

基金：

欧洲研究理事会;

关键词：

CATACLYSMIC VARIABLES; GALACTIC-CENTER; EMISSION; ACCRETION; BULGE; ORIGIN; SPECTROSCOPY; COUNTERPARTS; POPULATION; EXPLOSION;

D O I：

10.3847/1538-4357/ace90c

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report timing and broadband spectral analysis of a Galactic X-ray source, CXOGBS J174517.0-321356 (J1745), with a 614 s periodicity. Chandra discovered the source in the direction of the Galactic Bulge. Gong proposed that J1745 was either an intermediate polar (IP) with a mass of similar to 1 M circle dot, or an ultracompact X-ray binary (UCXB). To confirm J1745's nature, we jointly fit XMM-Newton and NuSTAR spectra, ruling out a UCXB origin. We have developed a physically realistic model that considers a finite magnetosphere radius, X-ray absorption from the preshock region, and reflection from the white-dwarf (WD) surface to properly determine the IP properties, especially its WD mass. To assess systematic errors on the WD mass measurement, we consider a broad range of specific accretion rates ( m=0.6-44 g cm-2 s-1) based on the uncertain source distance (d = 3-8 kpc) and fractional accretion area (f = 0.001-0.025). Our model properly implements the fitted accretion column height in the X-ray reflection model and accounts for the underestimated mass accretion rate due to the (unobserved) soft X-ray blackbody and cyclotron cooling emissions. We found that the lowest accretion rate of m = 0.6 g cm-2 s-1, which corresponds to the nearest source distance and maximum f value, yields a WD mass of (0.92 +/- 0.08)M circle dot. On the other hand, as long as the accretion rate is m greater than or similar to 3 g cm-2 s-1, the WD mass is robustly measured to be (0.81 +/- 0.06)M circle dot, nearly independent of m . The derived WD mass range is consistent with the mean WD mass of nearby IPs. Assuming spin equilibrium between the WD and accretion disk, we constrained the WD magnetic field to B greater than or similar to 7 MG, indicating that it could be a highly magnetized IP. Our analysis presents the most comprehensive methodology for constraining the WD mass and B field of an IP by consolidating the effects of cyclotron cooling, finite magnetospheric radius, and accretion column height.

引用

页数：14