Photoelectric observations of CC andromedae.

THE AGE OF THE DIRECTLY IMAGED PLANET HOST STAR k ANDROMEDAE DETERMINED FROM INTERFEROMETRIC OBSERVATIONS

κ Andromedae, an early-type star that hosts a directly imaged low-mass companion, is expected to be oblate due to its rapid rotational velocity (v sin i=∼162 km s). We observed the star with the CHARA Array’s optical beam combiner, PAVO, measuring its size at multiple orientations and determining its oblateness. The interferometric measurements, combined with photometry and this v sin i value a...

The Planetary System of Upsilon Andromedae

The bright F8 V solar-type star upsilon Andromedae has recently been reported to have a system of three planets of Jovian masses. In order to investigate the orbital stability and mutual gravitational interactions among these extrasolar planets, both forward and backward integrations from the latest observed orbital elements for all three planets' orbits have been performed under the coplanar a...

The Dwarf Nova Pq Andromedae

The Light Curve of S Andromedae

Historical observations of S And, in combination with the color versus rateof-decline relationship for well observed SN 1991bg-like supernovae, are used to estimate a rate of decline ∆m15 (B) = 2.21 and an intrinsic color at maximum [B(0)− V (0)]o = 1.32 for SN 1885A. Subject headings: supernovae:individual (S Andromedae)

Apsidal Alignment in Upsilon Andromedae

One of the parameters fitted by Doppler radial velocity measurements of extrasolar planetary systems is ω, the argument of pericenter of a given planet’s orbit referenced to the plane of the sky. Curiously, the ω’s of the outer two planets orbiting Upsilon Andromedae are presently nearly identical: ∆ω ≡ ωD − ωC = 4. 8 ± 4. 8 (1σ). This observation is least surprising if planets C and D occupy o...