Cyclotron emission, absorption, and the two faces of X-ray pulsar A 0535+262. (arXiv:1905.09496v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tsygankov_S/0/1/0/all/0/1">Sergey S. Tsygankov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doroshenko_V/0/1/0/all/0/1">Victor Doroshenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mushtukov_A/0/1/0/all/0/1">Alexander A. Mushtukov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suleimanov_V/0/1/0/all/0/1">Valery F. Suleimanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lutovinov_A/0/1/0/all/0/1">Alexander A. Lutovinov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poutanen_J/0/1/0/all/0/1">Juri Poutanen</a>
Deep NuSTAR observation of X-ray pulsar A 0535+262, performed at a very low
luminosity of $sim7times10^{34}$ erg s$^{-1}$, revealed the presence of two
spectral components. We argue that the high-energy component is associated with
cyclotron emission from recombination of electrons collisionally excited to the
upper Landau levels. The cyclotron line energy of $E_{rm cyc}=47.7pm0.8$ keV
was measured at the luminosity of almost an order of magnitude lower than what
was achieved before. The data firmly exclude a positive correlation of the
cyclotron energy with the mass accretion rate in this source.
Deep NuSTAR observation of X-ray pulsar A 0535+262, performed at a very low
luminosity of $sim7times10^{34}$ erg s$^{-1}$, revealed the presence of two
spectral components. We argue that the high-energy component is associated with
cyclotron emission from recombination of electrons collisionally excited to the
upper Landau levels. The cyclotron line energy of $E_{rm cyc}=47.7pm0.8$ keV
was measured at the luminosity of almost an order of magnitude lower than what
was achieved before. The data firmly exclude a positive correlation of the
cyclotron energy with the mass accretion rate in this source.
http://arxiv.org/icons/sfx.gif
