Sco X-1

Miyamoto, S.; Matsuoka, M.

doi:10.1007/bf02431834

Cited by 21 publications

(10 citation statements)

References 152 publications

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“…In other occasions the hard tail in Sco X-1 was not found, perhaps owing to pronounced variations (e.g. [55], and references therein). Evidence for a hard component was also found in Cyg X-2 [62] and GX 349+2 [29].…”

Section: A Few Words On Lmxrbsmentioning

confidence: 94%

Hard X-ray emission from neutron star X-ray binaries

Salvo

Santangelo

Segreto

2004

Nuclear Physics B - Proceedings Supplements

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Section: A Few Words On Lmxrbsmentioning

confidence: 94%

Hard X-ray emission from neutron star X-ray binaries

Salvo

Santangelo

Segreto

2004

Nuclear Physics B - Proceedings Supplements

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“…It seems that all BHCs in the low/hard state are observed to produce almost-continuous jets whose total power budget is likely to be a significant fraction (≥ 20%) of the total accretion energy (Fender 2001). All the Z sources are detected as variable radio sources, with the highest radio fluxes associated with the HB, gradually decreasing when the source moves to the NB and to the FB (Penninx et al 1988, Hasinger et al 1990, and this radio emission is again probably due to jets (e.g. Fender & Hendry 2000).…”

Section: Hard X-ray Emission From Z Sourcesmentioning

confidence: 99%

Hard X-ray Emission from Low Mass X-ray Binaries

Salvo¹,

Robba²

2003

Chin. J. Astron. Astrophys.

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In this paper we review our current knowledge of the hard X-ray emission properties of old accreting neutron stars in low mass X-ray binaries, with particular attention to recent results obtained for the brightest sources of this class, the so-called Z sources. While less luminous low mass X-ray binaries often show quite hard spectra, sometimes extending up to energies > ∼ 100 keV, the spectra of Z sources are always very soft, dominated by thermal components with characteristic temperatures ∼ 3 − 6 keV. However, recent broad band observations revealed the presence of a weak hard (power-law) component that is sometimes present in the spectra of these sources. These observations have strengthened the analogies between the spectral behavior of low mass X-ray binaries hosting neutron stars and binary systems containing black hole candidates. The physical parameters regulating the presence of this hard component are unknown yet. The first parameter may be the mass accretion rate, as indicated by the general anticorrelation between the fraction luminosity in hard X-rays and mass accretion rate apparent over different sources spanning a large range of luminosities as well as individual sources undergoing state changes. However, a second, yet unknown, parameter is probably needed to explain all the phenomenology. The broad high energy coverage and good sensitivity of the INTEGRAL mission can represent an important step forward in the understanding of the origin and properties of high energy components in accreting X-ray binaries.

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“…In contrast to the pulsating X-ray binaries, most of tale persistent sources which do not pulse, such as Sco X -1 (Miyamoto and Matsuoka 1977;Lamb and Sanford 1979;Coe at al. 1980;Johnson at al.…”

Section: Galactic Budge Sourcesmentioning

confidence: 99%