The giant outburst of EXO 2030+375

The Be X-ray binary EXO 2030+375 went through its third recorded giant outburst from June 2021 to early 2022. We present the results of both spectral and timing analysis based on NICER monitoring, covering the 2−10 keV flux range from 20 to 310 mCrab. Dense monitoring with observations carried out about every second day and a total exposure time of ∼160 ks allowed us to closely track the source evolution over the outburst. Changes in the spectral shape and pulse profiles showed a stable luminosity dependence during the rise and decline. The same type of dependence has been seen in past outbursts. The pulse profile is characterized by several distinct peaks and dips. The profiles show a clear dependence on luminosity with a stark transition at a luminosity of ∼2 × 10 36 erg s −1 , indicating a change in the emission pattern. Using relativistic raytracing, we demonstrate how anisotropic beaming of emission from an accretion channel with a constant geometrical configuration can give rise to the observed pulse profiles over a range of luminosities.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2024-08-01
DOI
https://doi.org/10.1051/0004-6361/202348594
Citations
7
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
2.32

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article

The giant outburst of EXO 2030+375

Pragati Pradhan, R. Staubert, J. Wilms, Brent West et al.
7 citations
Astronomy and Astrophysics
Gamma-ray bursts and supernovae
2.32
article

The giant outburst of EXO 2030+375

Pragati Pradhan, R. Staubert, J. Wilms, Brent West, Jakob Stierhof, E. Sokolova-Lapa, Gaurava K. Jaisawal, P. Kretschmar, R. Rothschild, P. Thalhammer, Peter A. Becker, A. Zainab, Joel B. Coley, Ralf Ballhausen, K. Pottschmidt
article en
7 citations

Abstract

The Be X-ray binary EXO 2030+375 went through its third recorded giant outburst from June 2021 to early 2022. We present the results of both spectral and timing analysis based on NICER monitoring, covering the 2−10 keV flux range from 20 to 310 mCrab. Dense monitoring with observations carried out about every second day and a total exposure time of ∼160 ks allowed us to closely track the source evolution over the outburst. Changes in the spectral shape and pulse profiles showed a stable luminosity dependence during the rise and decline. The same type of dependence has been seen in past outbursts. The pulse profile is characterized by several distinct peaks and dips. The profiles show a clear dependence on luminosity with a stark transition at a luminosity of ∼2 × 10 36 erg s −1 , indicating a change in the emission pattern. Using relativistic raytracing, we demonstrate how anisotropic beaming of emission from an accretion channel with a constant geometrical configuration can give rise to the observed pulse profiles over a range of luminosities.

Astronomy and AstrophysicsVol. 688
Vassar College (US), Goddard Space Flight Center (US), Howard University (US), George Mason University (US), Friedrich-Alexander-Universität Erlangen-Nürnberg (DE), United States Naval Academy (US), University of California San Diego (US), European Space Astronomy Centre (ES), Astrophysics Science Division (US), Massachusetts Institute of Technology (US), University of Maryland, College Park (US), University of Maryland, Baltimore County (US), University of Tübingen (DE), Embry–Riddle Aeronautical University (US), Technical University of Denmark (DK)
National Aeronautics and Space Administration, European Space Agency, Deutsche Forschungsgemeinschaft, Nuclear Safety and Security Commission, Goddard Space Flight Center
Openalex Percentile: Top 12%
Gamma-ray bursts and supernovae
2.32
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