Empirical effective temperatures and bolometric corrections for early-type stars

Code, A. D.; Bless, R. C.; Davis, John; Brown, Robert

doi:10.1086/154093

Cited by 325 publications

(291 citation statements)

References 0 publications

Supporting

Mentioning

252

Contrasting

Unclassified

Order By: Relevance

“…It is clear that the values of Code et al (1976) and Malagnini et al (1986) are the most accurate data for the normal star bolometric correction BC n (T eff ). Note that the BC values of Schmidt-Kaler, which are sometimes used for Ap stars (e.g., Hubrig et al 2000) are systematically too negative compared to the more accurate data of Code et al (1976) and Malagnini et al (1986), and differ from the calibration adopted here by about 0.25 mag.…”

Section: Bolometric Correctionsmentioning

confidence: 92%

“…We also plot the variation of bolometric correction BC n (T eff ) with T eff for normal stars, using (upper curve) Schmidt-Kaler's values (Lang 1992), and Balona's 1994 fit (middle curve) to the fundamental data of Code et al (1976) and of Malagnini et al (1986). (Lang 1992); the middle line is Balona's (1994) fit to the fundamental data of Code et al (1976) and Malagnini et al (1986), and the lowest curve is a polynomial fit to the Ap data as described in the text.…”

Section: Bolometric Correctionsmentioning

confidence: 99%

See 1 more Smart Citation

Searching for links between magnetic fields and stellar evolution

Landstreet¹,

Bagnulo²,

Andretta³

et al. 2007

A&A

175

249

View full text Add to dashboard Cite

Context. The evolution of magnetic fields in Ap stars during the main sequence phase is presently mostly unconstrained by observation because of the difficulty of assigning accurate ages to known field Ap stars. Aims. We are carrying out a large survey of magnetic fields in cluster Ap stars with the goal of obtaining a sample of these stars with well-determined ages. In this paper we analyse the information available from the survey as it currently stands. Methods. We select from the available observational sample the stars that are probably (1) cluster or association members and (2) magnetic Ap stars. For the stars in this subsample we determine the fundamental parameters T eff , L/L , and M/M . With these data and the cluster ages we assign both absolute age and fractional age (the fraction of the main sequence lifetime completed). For this purpose we have derived new bolometric corrections for Ap stars. Results. Magnetic fields are present at the surfaces of Ap stars from the ZAMS to the TAMS. Statistically for the stars with M > 3 M the fields decline with advancing age approximately as expected from flux conservation together with increased stellar radius, or perhaps even faster than this rate, on a time scale of about 3 × 10 7 yr. In contrast, lower mass stars show no compelling evidence for field decrease even on a timescale of several times 10 8 yr. Conclusions. Study of magnetic cluster stars is now a powerful tool for obtaining constraints on evolution of Ap stars through the main sequence. Enlarging the sample of known cluster magnetic stars, and obtaining more precise rms fields, will help to clarify the results obtained so far. Further field observations are in progress.

show abstract

Section: Bolometric Correctionsmentioning

confidence: 92%

Section: Bolometric Correctionsmentioning

confidence: 99%

Searching for links between magnetic fields and stellar evolution

Landstreet¹,

Bagnulo²,

Andretta³

et al. 2007

A&A

175

249

View full text Add to dashboard Cite

show abstract

“…The T e ff values, which we use in the present study, are mainly determined by a direct or semi-direct method. We took our data from Code et al (1976), Blackwell & Shallis (1977), Saxner Sz Hammerbàck (1985), Leggett et al (1986), Blackwell et al (1990), Malagnini et al (1990), Blackwell et al (1991) and Blackwell & Lynas-Gray (1994). To complete this sample, T e ff for a few stars were taken from Hauck (1985).…”

Section: Calibration Of Color Indices In Terms Of Teff For the Main-smentioning

confidence: 99%

“…The standard stars are roughly the same as those used in the paper NN90. The stars with a known T e fr are taken from Code et al (1976), Lanz (1987) and Leggett et al (1986) and those with a known log g are eclipsing binaries or nearby stars with a reliable surface gravity, as well as members of the Orion association whose log g is given by the internal structure models of Schaller et al (1992).…”

Section: -1 B-type Starsmentioning

confidence: 99%

Photometric calibrations of the effective temperature

Hauck¹,

Kunzli²

1996

Open Astronomy

View full text Add to dashboard Cite

show abstract

“…The standard value E(B-V)=0.05 was used for the galactic foreground extinction, and the value E(B-V)=0.10 was used for the LMC. The photometric data were de-reddened using the reddening law of Code et al (1976) and Leitherer and Wolf (1984) for the visual and infrared bands, respectively. For the Strömgren uvby measurements the absolute calibration was obtained from Gray (1998).…”

Section: Continuum Energy Distributionsmentioning

confidence: 99%

A Two-Temperature Model for LBVs

Guo

Shan

2004

Proc. IAU

View full text Add to dashboard Cite

Abstract. The continuum energy distributions of R127 and R110 in the outburst phase are fitted by use of a optically envelope model. Both stars show two peaks in the continuum energy distributions in which one lies in the short-wavelength range (near 1250Å) and the other in the optical band. We suggest that the fluxes in the UV and optical bands may have different origins: the UV flux comes from the central star and the optical flux comes from the expanded optically envelope. We construct such a model for LBVs with the use of two LTE atmosphere models with different temperatures, and find it to be in satisfactory agreement with the observed spectral energy distributions of R127 and R110.

show abstract

Empirical effective temperatures and bolometric corrections for early-type stars

Cited by 325 publications

References 0 publications

Searching for links between magnetic fields and stellar evolution

Searching for links between magnetic fields and stellar evolution

Photometric calibrations of the effective temperature

A Two-Temperature Model for LBVs

Contact Info

Product

Resources

About