Kinematics of O-B5 giants

Stellar Kinematics from Hipparcos Proper Motions

From Hipparcos proper motions, we have analyzed the local kinematics of the Milky Way from the young O-B5 stars, classical Cepheids, and the late-type K-M giants. Comparing the derived results, the kinematical discrepancies between each subset of stars have been analyzed, and the possible reasons for the kinematical di erences have been discussed.

Spectroscopic Survey of Red Giants in the SMC . I : Kinematics 1

We present a spectroscopic survey of 2046 red giant stars, distributed over the central 4 kpc×2 kpc of the Small Magellanic Cloud (SMC). After fitting and removing a small velocity gradient across the SMC (7.9 km s −1 deg −1 oriented at 10 • E of N), we measure an rms velocity scatter of 27.5 ± 0.5 km s −1. The line of sight velocity distribution is well-characterized by a Gaussian and the velo...

the shoulders of Giants

Giants of the British Isles

[email protected] Most countries and civilizations have stories about giants in their culture. In Greek and Roman times, Giants were an integral part of history. Ovid documents the story of Giants who once piled mountains up to the stars and were destroyed when Zeus hurled his thunderbolts at them. Homer, in his Odyssey, describes many Giants, often the Cyclops, including ...

Polarimetry of Li - rich giants ⋆

Context. Protoplanetary nebulae typically present non-spherical envelopes. The origin of such geometry is still controversial. There are indications that it may be carried over from an earlier phase of stellar evolution, such as the AGB phase. But how early in the star’s evolution does the non-spherical envelope appear? Aims. Li-rich giants show dusty circumstellar envelopes that can help answe...