We present high‐resolution spectroscopy of the variable Ca II H & K absorptions in the star β Pictoris. 313 spectra were obtained on 53 nights between 1994 November and 1996 December in order to characterize the behaviour of the lines and to test the falling evaporating bodies (FEB) scenario. Near‐continuous absorption activity was seen, including blueshifted features, one of which rivalled the strength of that reported in 1997 June by Crawford, Beust & Lagrange. Redshifted features at ∼ 5‐‐20 km s‐1 were present until the end of 1995, and are evocative of a year‐long stream of infalling bodies with typically 4‐‐5 objects in the line of sight. At higher velocities, features were shorter lived and generally broader and shallower. These correlations also apply to blueshifted features. On 1995 June 9 we detected a probable narrow, short‐lived feature at a redshift of ∼ 130 km s‐1. The FEB models predict that the strength of the H line may exceed the K line value as a body tracks across the stellar disc, but we have no convincing observation of this, although we did observe some events during which the H & K absorptions evolved differently.
Using improved techniques, high‐quality CCD uvbyVI photometry has been obtained for the eclipsing binary HV 982 in the Large Magellanic Cloud (LMC). International Ultraviolet Explorer ultraviolet spectrophotometry was also obtained. These data have been analysed using the Wilson–Devinney synthetic light‐curve code and Kurucz low‐metallicity model atmospheres as well as the EBOP code. The system is detached and the orbit is eccentric. Apsidal motion is detected with apsidal period 205 ± 7 yr. The effective temperatures of the components are found via flux fitting to be Teff,1 = 28 000 ± 5000 K and Teff,2 = 27 200 ± 5000 K. The large errors result from uncertainties over the appropriate interstellar extinction correction. The system plausibly comprises two ∼ 8 M stars of radius 6–7 R separated by ∼ 30 R. For pedagogical and historical interest, the near simultaneity of the eclipse minima at different wavelengths is used to constrain the constancy of the speed of light with wavelength and the mass of the photon, yielding mγ < 10−41 kg. Because of the great distance to HV 982, this limit is some 102 times smaller than previously achieved with eclipse timings, but it is nevertheless 10 orders of magnitude less stringent than that which is provided by satellite measurements of planetary magnetic fields.
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