English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

IGR J00370+6122 is a high-mass X-ray binary, of which the primary is a B1 Ibstar, whereas the companion is suggested to be a neutron star by the detectionof 346-s pulsation in one-off 4-ks observation. To better understand the natureof the compact companion, the present work performs timing and spectral studiesof the X-ray data of this object, taken with XMM-Newton, Swift, Suzaku, RXTE,and INTEGRAL. In the XMM-Newton data, a sign of coherent 674 s pulsation wasdetected, for which the previous 346-s period may be the 2nd harmonic. Thespectra exhibited the "harder when brighter" trend in the 1$-$10 keV range, anda flat continuum without clear cutoff in the 10$-$80 keV range. Theseproperties are both similar to those observed from several low-luminosityaccreting pulsars, including X Persei in particular. Thus, the compact objectin IGR J00370+6122 is considered to be a magnetized neutron star with a ratherlow luminosity. The orbital period was refined to $15.6649 \pm 0.0014$ d. Alongthe orbit, the luminosity changes by 3 orders of magnitude, involving a suddendrop from $\sim 4 \times 10^{33}$ to $\sim 1\times10^{32}$ erg s$^{-1}$ at anorbital phase of 0.3 (and probably vice verse at 0.95). Although thesephenomena cannot be explained by a simple Hoyle-Lyttleton accretion from theprimary's stellar winds, they can be explained when incorporating the propellereffect with a strong dipole magnetic field of $\sim 5 \times10^{13}$ G.Therefore, the neutron star in IGR J00370+6122 may have a stronger magneticfield compared to ordinary X-ray pulsars.

A study of the accretion mechanisms of the High Mass X-ray Binary IGR J00370+6122