Peritoneal Dialysis Access/Placement/Connectors

Piraino, Beth

doi:10.1007/978-0-585-36947-1_20

Cited by 4 publications

(4 citation statements)

References 197 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The photon index was 1.88 ± 0.05, the cutoff energy was 6.43 ± 0.15 keV, and the folding energy was 5.87 ± 0.20 keV. The cutoff energy is similar to that found for the X-ray pulsars GS 1843+00 (Piraino et al 2000) and SMC X-1 (Naik & Paul 2004), but the photon index is softer than found for those or other standard accreting X-ray pulsars. We attempted to fit the spectrum with a blackbody, the sum of a blackbody plus a power-law, and the sum of two blackbodies and a power-law, all with absorption, but were unable to obtain good fits with any of these models.…”

Section: Observations Of Hete J19001-2455supporting

confidence: 70%

Discovery of the Millisecond X‐Ray Pulsar HETE J1900.1−2455

Kaaret

Morgan

Vanderspek

et al. 2006

ApJ

View full text Add to dashboard Cite

We report the discovery of millisecond pulsations from the low-mass X-ray binary HETE J1900.1À2455, which was discovered by the detection of a type I X-ray burst by the High Energy Transient Explorer 2 (HETE-2). The neutron star emits coherent pulsations at 377.3 Hz and is in an 83.3 minute circular orbit with a companion of mass greater than 0.016 M and likely less than 0.07 M . The companion star's Roche lobe could be filled by a brown dwarf with no need for heating or nonstandard evolution. During one interval with an unusually high X-ray flux, the source produced quasi-periodic oscillations with a single peak at 883 Hz, and on subsequent days the pulsations were suppressed. We consider the distribution of spin versus orbital period in neutron star low-mass X-ray binaries.

show abstract

Section: Observations Of Hete J19001-2455supporting

confidence: 70%

Discovery of the Millisecond X‐Ray Pulsar HETE J1900.1−2455

Kaaret

Morgan

Vanderspek

et al. 2006

ApJ

View full text Add to dashboard Cite

show abstract

“…(9) ; (10) Liu, van Paradijs & van den Heuvel (2000); (11) Negueruela et al (1999); (12) Delgado-Marti et al (2001); (13) Yokogawa et al (2000a); (14) Negueruela et al (2000); (15) Borkus et al (1998); (16) Frontera et al (1985); (17) Kaaret et al (1999); (18) Cusumano et al (2000); (19) Corbet & Peele (1997); (20) Reig et al (2001); (21) Reig & Roche (1999a); (22) Wilson et al (1997b); (23) Petre & Gehrels (1994); (24) Reig & Roche (1999b); (25) Wilson, Finger & Scott (1999a); (26) Oosterbroek et al (1999);(27) in't Zand, Corbet & Marshall (2001b); (28) Kelley, Rappaport & Ayasli (1983); (29) Torii et al (1999); (30) Smith et al (1998); (31) Motch et al (1997); (32) Torii et al (1998); (33) Israel, Covino & Polcaro (2000). (34) Marshall, Lochner & Takeshima (1997); (35) Kinugasa et al (1998); (36) Israel et al (2001); (37) Piraino et al (2000); (38) Wilson et al (1997b); (39) Takeshima et al (1998); (40) Wilson et al (2003); (41) Paul et al (2001); (42) Tsygankov & Lutovinov (2005); (43) Negueruela et al (2003); (44) Reig, Negueruela & Fabregat (2001); (45) Wilson, Finger & Scott (1999b) the first emission-line star discovered by Angelo Secchi in 1866, and it ...…”

Section: Galactic Sources: Comments To the Tablementioning

confidence: 99%

“…Pulse fraction was obtained by BATSE (20-50 keV). Luminosity estimates are the following: 1) 2 • 10 36 erg s −1 (20-200 keV, 10 kpc) (Machanda 1999); 2) 3 • 10 37 erg s −1 (0.3-100 keV, 10 kpc) (Piraino et al 2000). 1845-024.…”

Section: Galactic Sources: Comments To the Tablementioning

confidence: 99%

Be–X-ray binaries and candidates

Raguzova¹,

Попов²

2005

Astronomical & Astrophysical Transactions

View full text Add to dashboard Cite

We present a compilative catalogue of Be/X-ray binaries and candidates in the Galaxy and in the Large and Small Magellanic Clouds. This catalogue contains 130 sources and provides information on names and spectral types of optical components, distances, spin characteristics of neutron stars, and on orbital and X-ray properties of binary systems. We give brief comments on each object and provide necessary references to original data.

show abstract

“…(o): [351]; X-ray obs. : [399,400,603]; hard X-ray outburst: [845,89]; possible cyclotron feature (B = 1.7×10 12 G): [512]; V−R = 2.1: [351]; distance ≥10 kpc: [351]; strong Hα emission: [351].…”

Section: Conclusion and Remarksmentioning

confidence: 99%

Catalogue of high-mass X-ray binaries in the Galaxy ($4^{th}$ edition)

Liu,

van Paradijs,

Heuvel

2007

Preprint

View full text Add to dashboard Cite

Aims. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (γ-rays, UV, optical, IR, radio). Methods. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.Results. We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries.

show abstract

Peritoneal Dialysis Access/Placement/Connectors

Cited by 4 publications

References 197 publications

Discovery of the Millisecond X‐Ray Pulsar HETE J1900.1−2455

Discovery of the Millisecond X‐Ray Pulsar HETE J1900.1−2455

Be–X-ray binaries and candidates

Catalogue of high-mass X-ray binaries in the Galaxy ($4^{th}$ edition)

Contact Info

Product

Resources

About