Effective Temperatures and Bolometric Corrections of Early-Type Stars

Morton, Donald C.; Adams, Thomas F.

doi:10.1086/149461

Cited by 133 publications

(42 citation statements)

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“…This formula has the advantage of not depending on the companion star radius. However, it does depend on the absolute magnitude M V , given in Martins & Plez (2006) for O-type stars and in Morton & Adams (1968) and Panagia (1973) for B stars. The results obtained with this second method are consistent with those using the first approach.…”

Section: Sed Fitting Proceduresmentioning

confidence: 99%

Distribution of High-Mass X-Ray Binaries in the Milky Way

Coleiro

Chaty

2013

ApJ

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Observations of the high-energy sky, particularly with the INTEGRAL satellite, have quadrupled the number of supergiant X-ray binaries observed in the Galaxy and revealed new populations of previously hidden high-mass X-ray binaries (HMXBs), raising new questions about their formation and evolution. The number of detected HMXBs of different types is now high enough to allow us to carry out a statistical analysis of their distribution in the Milky Way. For the first time, we derive the distance and absorption of a sample of HMXBs using a spectral energy distribution fitting procedure, and we examine the correlation with the distribution of star-forming complexes (SFCs) in the Galaxy. We show that HMXBs are clustered with SFCs with a typical cluster size of 0.3 ± 0.05 kpc and a characteristic distance between clusters of 1.7 ± 0.3 kpc. Furthermore, we present an investigation of the expected offset between the position of spiral arms and HMXBs, allowing us to constrain age and migration distance due to supernova kick for 13 sources. These new methods will allow us to assess the influence of the environment on these high-energy objects with unprecedented reliability.

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Section: Sed Fitting Proceduresmentioning

confidence: 99%

Distribution of High-Mass X-Ray Binaries in the Milky Way

Coleiro

Chaty

2013

ApJ

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“…The observational points in each B and V light curves were then combined into normal points and weighted directly according to the number of individual observations including in a point. The temperature of the primary component was taken from Morton & Adams (1968) as equal to 36 100 K, corresponding to the O 6.5 spectral class given by Pearce (1952). This temperature is in accord with the discussion in Hilditch et al (1996) and in Harries et al (1997).…”

Section: Photometric Solutionsmentioning

confidence: 99%

The early type contact binary system V 382 Cygni

Değirmenci

Sezer

Demirçan

et al. 1999

Astron. Astrophys. Suppl. Ser.

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Abstract. New photometric data set of the early type contact binary V 382 Cyg have been analyzed with emphasis on determining the photometric mass ratio of the system. The result (q = 0.68) supports the value given by Popper & Hill (1991). A study of the system using new data shows a period increase of about 3.28 s per century, which corresponds to a very large rate ∼ 5.0 10 −6 M /yr of mass transfer from the less massive to the more massive component under the conservative mass transfer hypothesis.

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“…However, the Hp amplitudes derived in°2. Morton & Adams (1968) were used instead of the Code et al (1976) calibration.…”

Section: The First Two Nightsmentioning

confidence: 99%

The δ Scuti Star DK Virginis (HR 5005) Revisited1

Jerzykiewicz¹,

Pamyatnykh

2000

PUBL ASTRON SOC PAC

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ABSTRACT. An analysis of Hp photometry of DK Virginis is carried out. The analysis reveals two frequencies, and cycles day~1. These values turn out to be good enough to bridge the f 1 \ 9.2095 f 2 \ 7.5764 gap between the two available series of ground-based data, obtained in 1973 and 1980, so that the frequencies can be reÐned. The reÐned values are equal to 9.20945 and 7.57641 cycles day~1. The corresponding V amplitudes amount to 8.6^0.4 and 11.1^0.4 mmag, and the epochs of maximum light are equal to 2,441,715.0294^0.0008 and 2,441,715.1205^0.0007. The synthetic light curve, computed with these JD _ parameters, correctly reproduces the large light range on JD 2,439,177, the night in 1966 when the star was discovered to be variable, and the small range on JD 2,440,682, when the light variation was not detected. In this way, all photometric observations of DK Vir are accounted for, indicating that the two frequencies have not changed appreciably since 1965, and that the V amplitudes were constant over the interval from 1965 to 1980.Using a photometric e †ective temperature and Hipparcos parallax, we plot the star in the H-R diagram. Comparison with evolutionary tracks then shows that DK Vir is at the end of the main-sequence stage of its evolution or slightly beyond, with a mass of 2.1 or somewhat smaller. Finally, an examination of linear M _ nonadiabatic pulsation frequencies of modes with l ¹ 2 indicates that the two observed modes cannot both be radial, and that the mode must be nonradial if the star is still on the main sequence. f 1 The properties of the Hipparcos spectral window are examined in the Appendix.

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Effective Temperatures and Bolometric Corrections of Early-Type Stars

Cited by 133 publications

References 0 publications

Distribution of High-Mass X-Ray Binaries in the Milky Way

Distribution of High-Mass X-Ray Binaries in the Milky Way

The early type contact binary system V 382 Cygni

The δ Scuti Star DK Virginis (HR 5005) Revisited1

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