A mathematical model of thermoelectronic laser energy conversion in moving plasma

Alekseeva, I. V.; Budnik, A. P.; Zherebtsov, V. A.; Zrodnikov, A. V.

doi:10.1134/1.1969771

Cited by 1 publication

(4 citation statements)

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“…We could not find any information on bandwidths used by the other authors. Nearly all the observations extend from 3200 A to about 8000 A, but Alekseeva et al (1997) and Glushnieva et al (1998a) obtained observations up to 10 800 A. For consistency with other observations, we ignored observations beyond 8500 A.…”

Section: Visual Observationsmentioning

confidence: 82%

“…301 stars appear in both catalogues. They were checked against the following catalogues of visual scans: Adelman et al (1989), Alekseeva et al (1996Alekseeva et al ( , 1997, Breger (1976), Burnashev (1985), Glushnieva et al (1998a,b) and Kharitonov, Tereshchenko & Knyazeva (1988). Observations exist for 137 stars from the previous sample in at least one of the visual catalogues.…”

Section: S E L E C T I O N O F S Ta R S a N D Data S O U R C E Smentioning

confidence: 99%

“…Other name Ad - Adelman et al (1989), Br -Breger (1976), Bu -Burnashev (1985), Gl - Glushnieva et al (1998b), Kh -Kharitonov et al (1988). a Three more visual scans from Alekseeva et al (1996Alekseeva et al ( , 1997 and Glushnieva et al (1998a) were also included.…”

Section: Hdmentioning

confidence: 99%

“…In the catalogues of Alekseeva et al (1997), Burnashev (1985), Glushnieva et al (1998a,b) and Kharitonov et al (1988) (henceforth ABGK catalogues) from one to seven scans per star are given. Alekseeva et al (1997) used the bandwidth of 100 A. We could not find any information on bandwidths used by the other authors.…”

Section: Visual Observationsmentioning

confidence: 99%

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Effective temperatures of magnetic chemically peculiar stars from full spectral energy distributions

Lipski

Stępień

2008

Monthly Notices of the Royal Astronomical Society

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New determinations of effective temperatures of 23 magnetic, chemically peculiar (mCP) stars were obtained from a fit of metal‐enhanced model atmospheres to the observed spectral energy distributions (SED) from ultraviolet (UV) to red. Temperatures of four more CP stars without magnetic measurements were also obtained, of which three show light variations characteristic of magnetic variables, and the fourth may possibly be normal. The root‐mean‐square (rms) method was used to fit the theoretical SED to the observations corrected for reddening if necessary, with metallicity and effective temperature as the fitting parameters. Gravity was assumed to be equal to log g= 4 for main‐sequence stars and to log g= 3 for two giants in the considered sample. Equal weights were given to the UV part and visual part of SED. An attempt was made to obtain a three‐parameter fit (with reddening included) to the observed SED of HD 215441. It turned out that the three‐parameter fit gave spurious results due to correlations among the parameters. We could determine the reddening of that star only by assuming that the metallicity of the model is known, hence reducing the number of fitting parameters to two. Independently of the formal quality of fit resulting from the rms method applied to the whole SED, the quality of fit was additionally checked for each star by determination of the temperature from the best‐fitting model atmosphere to the UV part and the visual part of SED separately. Both temperatures should be close to one another if the global best‐fitting model satisfactorily describes the full observed SED. This is the case for about a half of the investigated stars but the difference exceeds 750 K for the remaining stars with the extreme values above 2000 K. Possible reasons for such discrepancies are discussed. New revised calibrations of effective temperature and bolometric corrections of mCP stars in terms of reddening free Strömgren indices are given.

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Section: Visual Observationsmentioning

confidence: 82%