The Balmer Wavelength Range of BP Tauri

Details The Balmer Wavelength Range of BP Tauri The Balmer Wavelength Range of BP Tauri

2000-03-22

arxiv.org/abs/astro-ph/0003313v1

Astronomy and Astrophysics

Astrophysics

34 pages, 3 tables, 11 figures. Accepted in the Astrophysical Journal

Scientific paper

10.1086/309253

We have analyzed all the observations of BP Tauri taken by the International Ultraviolet Explorer in the low resolution (6 A), long wavelength (from 1850 to 3350 A) range. This dataset contains 61 spectra. These spectra do not show any correlation between the continuum flux and the MgII line flux, thus resolving a standing controversy in the literature concerning the origin of the MgII line flux. There is no correlation between the color temperature of the UV continuum and the average value of its flux. Using models of the accretion process developed by Calvet & Gullbring (1998), we obtain energy fluxes, accretion spot sizes, and accretion rates from the IUE observations of BP Tauri. We find average energy fluxes of 5.0 10^11 ergs cm^{-2} s^{-1}, average spot sizes of 4.4 10^{-3} times the stellar surface, and average accretion rates of 1.6 10^-8 msun/yr. Our analysis shows that the particle energy flux and the UV flux in the stellar surface are proportional to each other. Most strikingly, we observe a correlation between accretion rate and spot size, with the spot size increasing as the square of the accretion rate. Based on the results of a simulation, we conclude that geometrical effects are not enough to account for this effect. Current models of the accretion process fail to reproduce such an effect, suggesting the need of using more realistic descriptions of the stellar field when treating magnetospheric accretion. There may also be an unmodelled efficiency factor that determines how matter is loaded into the field lines.

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