Advanced Mass Spectrometry of Lubricants

Campana, Joseph E.; Freas, R. B.

doi:10.1080/05698198608981683

Cited by 105 publications

(174 citation statements)

References 13 publications

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“…While our spectrophotometry of stars L, C, and F agrees well with our own photometry, it disagrees with measurements in the literature: the synthetic V -band magnitudes are 0.4 mag brighter than both the V -band magnitudes of Neuhäuser et al (1997) and the V -band magnitudes inferred from Gunn g and r measurements of Campana et al (1997) Comparing colours, we find that our synthetic B − V and V − R colours are systematically redder and bluer, respectively, than those of Neuhäuser et al (1997). The inferred B −R values, however, are consistent.…”

Section: Previous Photometry Of Stars L C and Fsupporting

confidence: 56%

“…For all three, our colours are consistent with the spectral types (for a small amount of reddening; see Sect. 5), while the B − V and V − R (but not B − R) colours of Neuhäuser et al (1997) and the g − r colour of Campana et al (1997) are inconsistent with the spectral types (independent of reddening). We thus conclude that, despite the inconsistencies with earlier work, our calibration is reliable.…”

Section: Previous Photometry Of Stars L C and Fmentioning

confidence: 85%

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Optical spectroscopy and photometry of the neutron star RX J1856.5-3754

Kerkwijk

Kulkarni²

2001

A&A

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Abstract. We present spectroscopy and imaging with the Very Large Telescope (VLT) of the neutron star RX J1856.5-3754. Little is known about the nature of this source other than that it is a nearby hot neutron star. Our VLT spectrum does not show any strong emission or absorption features. With considerable care to photometric calibration, we obtain photometric measurements over the optical and ultra-violet (UV) using our VLT observations and a detailed analysis of archival Hubble Space Telescope data. We find that the entire optical to UV spectral energy distribution is well described by a slightly reddened Rayleigh-Jeans tailwhere A λ /AV is the reddening curve; implied V = 25.58 ± 0.02). The reddening is consistent with the interstellar absorption inferred from X-ray spectroscopy. The simplest explanation for this Rayleigh-Jeans emission is that the optical-UV radiation arises from thermal emission from the surface of the neutron star. The high degree to which the data conform to the Rayleigh-Jeans tail significantly limits contributions from other sources of emission. In particular, our observations are inconsistent with the presence of an accretion disk and also strongly constrain the amount of magnetospheric emission from this enigmatic neutron star.

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Section: Previous Photometry Of Stars L C and Fsupporting

confidence: 56%

Section: Previous Photometry Of Stars L C and Fmentioning

confidence: 85%

Optical spectroscopy and photometry of the neutron star RX J1856.5-3754

Kerkwijk

Kulkarni²

2001

A&A

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“…Since these objects have a short lifetime (∼10 6 yr), it is expected that GRB explosions take place close to or inside the original star forming regions, where a dense circumburst medium is present. Thus, high level of absorption is expected, and this is consistent with the observations in (∼50 per cent) of Swift bursts (Campana et al 2005; O'Brien et al 2005).…”

Section: Discussionsupporting

confidence: 90%

Swift observations of GRB 050712

Pasquale

Grupe

Poole

et al. 2006

Monthly Notices of the Royal Astronomical Society

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We present the results of X‐ray and optical observations of GRB 050712 performed by Swift. The X‐ray light curve of this burst exhibits episodes of flares in the first 1000 s, the same epoch at which the UVOT detected an optical counterpart. A shallow X‐ray decay, with a decay slope of α=−0.73, followed and lasted ∼70 ks. This behaviour can be explained in terms of activity of the gamma‐ray burst ‘inner engine’, with the possibility that the last flare is caused by the interaction of the ejecta with the surrounding medium. We also find interesting spectral parameters for the X‐ray emission. In particular, data suggest the presence of an intrinsic absorption in the first 1000 s, which can be explained if circumburst medium clouds lie along the line of sight.

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“…Reassessments of RX J1856.5–3754 published by Campana, Mereghetti & Sidoli (1997) and Neuhäuser et al (1997) both confirm this conclusion, and Walter & Matthews (1997) have now identified a faint optical counterpart at magnitude 25.6, consistent with a neutron star. However, it has not been possible to distinguish between a `middle‐aged' pulsar like Geminga and an old neutron star accreting from the ISM.…”

Section: The Candidate Neutron Starsmentioning

confidence: 55%

The implications of radio-quiet neutron stars

Brazier

Johnston

1999

Monthly Notices of the Royal Astronomical Society

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We collate the evidence for rotation-powered neutron stars that are visible as X-ray sources and not as radio pulsars. Quantitative upper limits exist for the radio fluxes of eight objects, revealing a population at least an order of magnitude less luminous at radio wavelengths than known radio pulsars of similar power or age. These objects could have intrinsically low radio luminosities, but a simple alternative explanation is that they are pulsars in which the radio beams are directed away from Earth. Where hard X-ray or gamma-ray fluxes are seen, the beaming explanation implies different emission sites for the high-energy radiation and the unseen radio beams. We estimate that (a) the radio beaming fraction of young pulsars is roughly 50%, certainly much less than 100%, and (b) one neutron star is born in the Galaxy every ~90 years. We conclude that probably all neutron stars are born as radio pulsars and that most young, nearby pulsars have already been discovered.Comment: 10 pages, 2 figures, TeX, uses mn.tex, submitted Oct 97 to MNRAS, waiting for referee's repor

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Advanced Mass Spectrometry of Lubricants

Cited by 105 publications

References 13 publications

Optical spectroscopy and photometry of the neutron star RX J1856.5-3754

Optical spectroscopy and photometry of the neutron star RX J1856.5-3754

Swift observations of GRB 050712

The implications of radio-quiet neutron stars

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