Magnetic Fields of Neutron Stars in X-Ray Binaries

Revnivtsev, M.; Mereghetti, S.

doi:10.1007/978-1-4939-3550-5_9

Cited by 8 publications

(7 citation statements)

References 159 publications

(195 reference statements)

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“…All ∼ 30 known magnetars (or "candidate" magnetars) are isolated neutron stars (Olausen and Kaspi, 2014). Conversely, all neutron stars in X-ray binaries are observed to have magnetic field strengths < 10 13 G, below the magnetar range (see, e.g., Revnivtsev and Mereghetti, 2016).…”

Section: Pulxs As Magnetars In Binary Systemsmentioning

confidence: 99%

Ultraluminous X-ray sources

King

Lasota

Middleton

2023

New Astronomy Reviews

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Section: Pulxs As Magnetars In Binary Systemsmentioning

confidence: 99%

Ultraluminous X-ray sources

King

Lasota

Middleton

2023

New Astronomy Reviews

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“…In the last 40 years the number of known electron cyclotron sources has increased to ∼36 (see Table 4) due to investigations with many X-ray observatories like Ginga, MIR-HEXE, RXTE, BeppoSAX, INTEGRAL, Suzaku, and NuSTAR. For previous reviews about cyclotron line sources, see for example, Coburn et al (2002); Staubert (2003); Heindl et al (2004); Terada et al (2007); Wilms (2012); Caballero & Wilms (2012); Revnivtsev & Mereghetti (2016); Maitra (2017). Lists of CRSF sources can also be found at the webpages of Dr. Remeis-Sternwarte, Bamberg 1 and the Istituto Astrrofisica Spaziale, Bologna 2 .…”

Section: Introductionmentioning

confidence: 99%

Cyclotron lines in highly magnetized neutron stars

Staubert

Trümper

Kendziorra

et al. 2019

A&A

222

221

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Cyclotron lines, also called cyclotron resonant scattering features (CRSF) are spectral features, generally appearing in absorption, in the X-ray spectra of objects containing highly magnetized neutron stars, allowing the direct measurement of the magnetic field strength in these objects. Cyclotron features are thought to be due to resonant scattering of photons by electrons in the strong magnetic fields. The main content of this contribution focusses on electron cyclotron lines as found in accreting X-ray binary pulsars (XRBP) with magnetic fields on the order of several 10 12 Gauss. Also, possible proton cyclotron lines from single neutron stars with even stronger magnetic fields are briefly discussed. With regard to electron cyclotron lines, we present an updated list of XRBPs that show evidence of such absorption lines. The first such line was discovered in a 1976 balloon observation of the accreting binary pulsar Hercules X-1, it is considered to be the first direct measurement of the magnetic field of a neutron star. As of today (mid 2018), we list 36 XRBPs showing evidence of one ore more electron cyclotron absorption line(s). A few have been measured only once and must be confirmed (several more objects are listed as candidates). In addition to the Tables of objects, we summarize the evidence of variability of the cyclotron line as a function of various parameters (especially pulse phase, luminosity and time), and add a discussion of the different observed phenomena and associated attempts of theoretical modeling. We also discuss our understanding of the underlying physics of accretion onto highly magnetized neutron stars. For proton cyclotron lines, we present tables with seven neutron stars and discuss their nature and the physics in these objects.

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“…In contrast to other ways of estimating such a magnetic field strength, no further model assumptions are needed. We now know about 35 binary X-ray pulsars that show cyclotron lines in their spectra, generally between a few keV and ∼100 keV (for reviews, see Staubert et al 2019;Revnivtsev & Mereghetti 2016;Caballero & Wilms 2012;Wilms 2012;Terada et al 2007;Heindl et al 2004;Staubert 2003;Coburn et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Cyclotron line energy in Hercules X-1: stable after the decay

Staubert

Ducci

et al. 2020

A&A

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We summarize the results of a dedicated effort made between 2012 and 2019 to follow the evolution of the cyclotron line in Her X-1 through repeated NuSTAR observations. The previously observed nearly 20-year-long decay of the cyclotron line energy has ended in 2012: from then on, the pulse-phase-averaged flux-corrected cyclotron line energy has remained stable and constant at an average value of Ecyc = (37.44 ± 0.07) keV (normalized to a flux level of 6.8 RXTE/ASM-cts s−1). The flux dependence of Ecyc discovered in 2007 is now measured with high precision, giving a slope of (0.675 ± 0.075) keV/(ASM-cts s−1), corresponding to an increase of 6.5% of Ecyc for an increase in flux by a factor of two. We also find that all line parameters as well as the continuum parameters show a correlation with X-ray flux. While a correlation between Ecyc and X-ray flux (both positive and negative) is now known for several accreting binaries with various suggestions for the underlying physics, the phenomenon of a long-term decay has so far only been seen in Her X-1 and Vela X-1, with far less convincing explanations.

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Magnetic Fields of Neutron Stars in X-Ray Binaries

Cited by 8 publications

References 159 publications

Ultraluminous X-ray sources

Ultraluminous X-ray sources

Cyclotron lines in highly magnetized neutron stars

Cyclotron line energy in Hercules X-1: stable after the decay

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