NGC 300 ULX1: spin evolution, super-Eddington accretion, and outflows-Reference-Cited by-同舟云学术

NGC 300 ULX1: spin evolution, super-Eddington accretion, and outflows

Published:2019-08-05 Issue:4 Volume:488 Page:5225-5231
ISSN:0035-8711
Container-title:Monthly Notices of the Royal Astronomical Society
language:en
Short-container-title:

Author:

Vasilopoulos G¹^ORCID,Petropoulou M²^ORCID,Koliopanos F³,Ray P S⁴^ORCID,Bailyn C B¹,Haberl F⁵,Gendreau K⁶

Affiliation:

1. Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA

2. Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA

3. IRAP, CNRS, 9 avenue du Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France

4. Space Science Division, U.S. Naval Research Laboratory, Washington, DC 20375, USA

5. Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany

6. X-Ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

Abstract

Abstract NGC 300 ULX1 is an ultraluminous X-ray pulsar, showing an unprecedented spin evolution, from about 126 s to less than 20 s in only 4 yr, consistent with steady mass accretion rate. Following its discovery we have been monitoring the system with Swift and NICER to further study its properties. We found that even though the observed flux of the system dropped by a factor of ≳20, the spin-up rate remained almost constant. A possible explanation is that the decrease in the observed flux is a result of increased absorption of obscuring material due to outflows or a precessing accretion disc.

Funder

Lyman Jr. Spitzer Postdoctoral Fellowship and Fermi Guest Investigator

U.S. Naval Research Laboratory

National Aeronautics and Space Administration

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Link

http://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stz2045/29100714/stz2045.pdf

Reference43 articles.

1. Optically Thick Outflows of Supercritical Accretion Discs: Radiative Diffusion Approach