Photograph of the Nebula П 240 Pegasi

The Visual Orbit of • Pegasi

We have determined the visual orbit for the spectroscopic binary • Pegasi with interferometric visibility data obtained by the Palomar Testbed Interferometer in 1997. • Peg is a double-lined binary system whose minimum masses and spectral typing suggests the possibility of eclipses. Our orbital and component diameter determinations do not favor the eclipse hypothesis : the limb-to-limb separati...

The Planet around 51 Pegasi

Doppler measurements of 51 Pegasi have been made from 1995 October through 1996 August, with a precision of 5 m s~1. We Ðnd a period of 4.231 days, a velocity amplitude of 56^ 1 m s~1, and a velocity curve that is essentially sinusoidal, all in excellent agreement with Mayor & Queloz. The only viable interpretation is a companion having minimum mass, m sin i \ 0.45 in a circular orbit of MJupit...

Calibration of ι Pegasi system

Recent observations provide determinations of individual masses, chemical composition and metallicity of the components of the spectroscopic and interferometric binary ι Peg (Boden et al. 1999). Using updated physics, to calibrate the system, we have computed using the stellar evolutionary code CESAM (Morel 1997), evolutionary sequences of stellar models with the masses of ι Peg A 1.326M and ι ...

The Continuing Slow Decline of AG Pegasi

We analyze optical and ultraviolet observations of the symbiotic binary AG Pegasi acquired during 1992–97. The bolometric luminosity of the hot component declined by a factor of 2–3 from 1980–1985 to 1997. Since 1992, the effective temperature of the hot component may have declined by 10%–20%, but this decline is comparable to the measurement errors. Optical observations of Hβ and He I emission...

A Musical Photograph?