Nietzsche's Great Style: Educator Of The Ears And Of The Heart

Crawford, Claudia

doi:10.1515/9783112418543-010

Cited by 3 publications

(3 citation statements)

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“…Smith & Balona (2006) did not observe the 1.77 d period in their optical photometry but report a possible 130 d period. Codina et al (1984) also note a strong polarization of the light from HD 110432 in observations made with a photopolarimeter attached to the 1.6-m telescope of the Brazilian Astrophysical Observatory (OAB) in Brasopolis, however they attribute most of the polarization to the star's proximity to the southern Coalsack dark nebula which is between the star and the Earth (Crawford, 1991). Radial velocities were observed to vary between 27 and 70 km s −1 by Buscombe (1962), likely based on moving emission lines; Smith & Balona (2006) adopt the latest value of 6 km s −1 from Thackeray et al (1973), which is confirmed by their own measurements, for their work.…”

Section: Resultsmentioning

confidence: 99%

Photometric observations of three high mass X-ray binaries and a search for variations induced by orbital motion

Sarty¹,

Pilecki²,

Reichart³

et al. 2011

Res. Astron. Astrophys.

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We searched for long period variation in V -band, I C -band and RXTE X-ray light curves of the High Mass X-ray Binaries (HMXBs) LS 1698 / RX J1037.5−5647, HD 110432 / 1H 1249−637 and HD 161103 / RX J1744.7−2713 in an attempt to discover orbitally induced variation. Data were obtained primarily from the ASAS database and were supplemented by shorter term observations made with the 24-and 40-inch ANU telescopes and one of the robotic PROMPT telescopes. Fourier periodograms suggested the existence of long period variation in the V -band light curves of all three HMXBs, however folding the data at those periods did not reveal convincing periodic variation. At this point we cannot rule out the existence of long term V -band variation for these three sources and hints of longer term variation may be seen in the higher precision PROMPT data. Long term V -band observations, on the order of several years, taken at a frequency of at least once per week and with a precision of 0.01 mag, therefore still have a chance of revealing long term variation in these three HMXBs.

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Section: Resultsmentioning

confidence: 99%

Photometric observations of three high mass X-ray binaries and a search for variations induced by orbital motion

Sarty¹,

Pilecki²,

Reichart³

et al. 2011

Res. Astron. Astrophys.

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show abstract

“…The spectrum appears to be contaminated with Ca II (3933 Å) and Na D. Although these features usually indicate the presence of a cooler companion, we expect some level of interstellar absorption given the extremely low galactic latitude (-0.94 deg) of CS 1246. Moreover, both Ca and Na D have been observed in the spectra of other stars located in and behind the Coalsack (Franco 2000(Franco , 1989Crawford 1991). No other spectral features indicative of a companion are present, and we currently have no reason to believe the lines originate from a companion star.…”

Section: The Mean Spectrummentioning

confidence: 97%

Photometry and spectroscopy of the new sdBV CS 1246

Barlow

Dunlap

Clemens

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We report the discovery of a large-amplitude oscillation in the hot subdwarf B star CS 1246 and present multi-colour photometry and time-resolved spectroscopy supporting this discovery. We used the 0.41-m PROMPT array to acquire data in the u', g', r', and i' filters simultaneously over 3 consecutive nights in 2009 April. These data reveal a single oscillation mode with a period of 371.707 +/- 0.002 s and an amplitude dependent upon wavelength, with a value of 34.5 +/- 1.6 mma in the u' filter. We detected no additional frequencies in any of the light curves. Subsequently, we used the 4.1-m SOAR telescope to acquire a time-series of 248 low-resolution spectra spanning 6 hrs to look for line profile variations. Models fits to the spectra give mean atmospheric values of Teff = 28450 +/- 700 K and log g = 5.46 +/- 0.11 undergoing variations with semi-amplitudes of 507 +/- 55 K and 0.034 +/- 0.009 dex, respectively. We also detect a radial velocity oscillation with an amplitude of 8.8 +/- 1.1 km/s. The relationship between the angular and physical radii variations shows the oscillation is consistent with a radial mode. Under the assumption of a radial pulsation, we compute the stellar distance, radius, and mass as d = 460 +/- 140 pc, R = 0.19 +/- 0.08 Rsun, and M = 0.39 +/- 0.22 Msun, respectively, using the Baade-Wesselink method.Comment: 12 pages, 11 figures, 3 tables. Accepted for publication in MNRA

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“…(o): [778]; Be star: [810]; UV obs. : [111]; interstellar absorption lines: [149]; optical obs. : [155,212]; variable radial velocity: [73]; distance of 0.3 kpc: [94]; 14 ks period: [771]; a Be/WD candidate?…”

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

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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.

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Nietzsche's Great Style: Educator Of The Ears And Of The Heart

Cited by 3 publications

References 0 publications

Photometric observations of three high mass X-ray binaries and a search for variations induced by orbital motion

Photometric observations of three high mass X-ray binaries and a search for variations induced by orbital motion

Photometry and spectroscopy of the new sdBV CS 1246

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

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