Spindown of neutron stars in close binary systems - II

Davies, R. E.; Pringle, J. E.

doi:10.1093/mnras/196.2.209

Cited by 166 publications

(208 citation statements)

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“…One can note that the magnetic dipole moment µ and the accretion rateṀ c always appear in the same combination, y =Ṁ c µ 2 , as was first noticed by Davies & Pringle (1981). Analysis of the nature of interaction of a magnetized star with the surrounding plasma allows us to write an approximate evolution equation for the angular momentum of a magnetic rotator in the general form (Lipunov (1982a)) dIω dt =Ṁk su − κ t µ 2 R 3 t , where k su is a specific angular momentum applied by the accretion matter to the rotator and R t is a radius of the interaction.…”

supporting

confidence: 68%

Population synthesis of binary relativistic stars

Липунов

2005

Proc. IAU

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supporting

confidence: 68%

Population synthesis of binary relativistic stars

Липунов

2005

Proc. IAU

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Section: X-ray Behaviourmentioning

confidence: 99%

“…Davies & Pringle 1981;Henrichs 1983). Four distinct phases of neutron star spindown in close binary systems have been proposed to be applicable to a particular range of rotation periods: pulsar-like, very rapid rotator, supersonic propeller, and subsonic propeller (Davies & Pringle 1981). According to these long-period neutron stars such as SAX J2103.5+4545 achieve the most effective braking during the subsonic propeller regimen, in which the rotational rate decelerates because of the interaction between the magnetosphere and the surrounding hot, quasi-static plasma envelope (Ikhsanov & Choi 2006).…”

Section: X-ray Behaviourmentioning

confidence: 99%

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

Camero

Zurita

Gutiérrez‐Soto

et al. 2014

A&A

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Aims. We present a multiwavelength study of the Be/X-ray binary system SAX J2103.5+4545 with the goal of better characterizing the transient behaviour of this source. Methods. SAX J2103.5+4545 was observed by Swift/XRT four times in 2007 from April 25 to May 5, and during quiescence in 2012 August 31. In addition, this source has been monitored from the ground-based astronomical observatories of El Teide (Tenerife, Spain), Roque de los Muchachos (La Palma, Spain), and Sierra Nevada (Granada, Spain) since 2011 August, and from the TÜBİTAK National Observatory (Antalya, Turkey) since 2009 June. We performed spectral and photometric temporal analyses to investigate the different states exhibited by SAX J2103.5+4545. Results. In X-rays, an absorbed power-law model provided the best fit for all the XRT spectra. An iron-line feature at ∼6.42 keV was present in all the observations except for that taken during quiescence in 2012. The photon indexes are consistent with previous studies of SAX J2103.5+4545 in high/low-luminosity states. Pulsations were found in all the XRT data from 2007 (2.839(2) mHz; MJD 54 222.02), but not during quiescence. The two optical outbursts in 2010 and 2012 lasted for about eight or nine months (as the one in 2007 probably did and the current one in 2014 might do) and were most probably caused by mass-ejection events from the Be star that eventually fed the circumstellar disc. All of these outbursts started about three months before the triggering of the X-ray activity, and at about the same period before the maximum of the Hα line equivalent width (in emission) was reached at only ∼-5 Å. The global correlation between the BV variability and the X-ray intensity was also observed at longer wavelengths in the IR domain.

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“…In a pre-low-mass X-ray Binary (pre-LMXB: see above), the newborn, fast-rotating neutron star is unable at first to accrete the matter that is being transferred from the companion through the inner Lagrangian point L 1 , because of the fast rotation of the neutron star (IS75, Davies et al 1979;Davies & Pringle 1981;Illarionov & Kompaneets 1990;Mineshige et al 1991;Illarionov et al 1993, G95, LRB99;Romanova et al 2004, RUKL05, UKRL06). Because of its large angular momentum, this matter forms an accretion disk and reaches the magnetospheric boundary of the magnetized neutron star, whereupon this ionized matter interacts with the fast-rotating neutron star's magnetic field, and the energy and angular momentum deposited in it by magnetic stresses associated with this fast-rotating magnetic field expel it.…”

Section: Propeller Phase In Pre-lmxbsmentioning

confidence: 99%

“…The 6.67 h periodicity is identified in our model with the orbital period of the binary. In our model the young neutron star is still spinning very rapidly, with a canonical spin period ∼10−100 ms, and is operating in the "propeller" regime, wherein any matter approaching the fast-rotating magnetosphere of the neutron star is expelled by the energy and angular momentum deposited into it through its interaction with the magnetospheric boundary (Illarionov & Sunyaev 1975, henceforth IS75;Davies et al 1979;Davies & Pringle 1981;Illarionov & Kompaneets 1990; Article published by EDP Sciences Mineshige et al 1991;Illarionov et al 1993;Ghosh 1995, and references therein, henceforth G95; Lovelace et al 1999, henceforth LRB99; Romanova et al 2004Romanova et al , 2005, henceforth RUKL05; Ustyugova et al 2006, henceforth UKRL06).…”

Section: Introductionmentioning

confidence: 99%

Young pre-low-mass X-ray binaries in the propeller phase

Bhadkamkar

Ghosh

2009

A&A

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Context. Discovery of the 6.7-h periodicity in the X-ray source 1E 161348-5055 in RCW 103 has led to investigations of the nature of this periodicity. Aims. To explore a model for 1E 161348-5055 wherein a fast-spinning neutron star with a magnetic field ∼10 12 G in a young prelow-mass X-ray Binary (pre-LMXB) with an eccentric orbit of period 6.7 h operates in the "propeller" phase. Methods. The 6.7-h light curve of 1E 161348-5055 is modeled in terms of orbitally-modulated mass transfer through a viscous accretion disk and subsequent propeller emission. Formation of eccentric binaries in supernovae and their subsequent tidal evolution are studied.Results. The light curve of 1E 161348-5055 can be quantitatively accounted for by models of propeller torques of both IllarionovSunyaev type and Romanova-Lovelace et al. type, and spectral and other properties are also in agreement. Formation and evolution of model systems are shown to be in accordance both with standard theories and with X-ray observations of 1E 161348-5055. Conclusions. The pre-LMXB model for 1E 161348-5055 and similar sources agrees with observation. Distinguishing features between this model and the recently-proposed magnetar model need to be explored.

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Spindown of neutron stars in close binary systems - II

Cited by 166 publications

References 0 publications

Population synthesis of binary relativistic stars

Population synthesis of binary relativistic stars

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

Young pre-low-mass X-ray binaries in the propeller phase

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