Large Space Velocity Research Articles

Is Cir X-1 a runaway binary?

RUNAWAY stars are produced when there is a supernova explosion in a close binary system. Usually such an explosion disrupts the binary system, but Gott1 has suggested that in a significant fraction of such supernovae the collapsed residue of the explosion may be retained in orbit around the runaway second star, the resultant system being a binary with high eccentricity and large space velocity. We suggest here that Cir X-1 is such a system.

Intercomparison of Space Velocities and Dispersions of Mira Variables with Those of Other Stars.

view Abstract Citations References Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Intercomparison of Space Velocities and Dispersions of Mira Variables with Those of Other Stars. Osvalds, V. Abstract After Wilson and Merrill (1942, Astrophys. J. 95, 248) the space velocities of Mira variables had been studied by P. G. Kulikovsky [1948, Var. Star Bull. (Russia) 6, 225], J. Ikaunieks (1950, Fiz. un Mat. Inst. Raksti, Riga II, 101), and U. S. Safronov [1955, Var. Star Bull. (Russia) 10, 236]. The numerical values for velocities and dispersions derived by us agree satisfactorily with those by the others with exception of the a component for variables with P >300 days. In our solution it is about 30 km/sec larger. The exceptionally high absolute magnitude and the large space velocity of the second subgroup, 150 ~ P ~ 200 days remain as in previous results and the cause for that is the large radial velocities in this group. It is interesting to analyze our results in the way suggested to us by Dr. Vyssotsky, as outlined in his summarizing article (1957, Publs. Astron. Soc. Pacific 69, 109). The position of subgroup 2 in the Haas-Bottlinger diagram indicates a high eccentricity of the orbits the stars in this group are describing. In addition, this group lags behind the galactic rotation much more than any of the other subgroups. Further, the proj ections of velocity-vector points on the galactic plane indicate a high orbital inclination for variables with periods ~ 300 days and a low inclination for those with P> 300 days. Also, the deviation of vertex and smaller group velocity indicates that the variables with P> 300 days stay closer to the galactic plane. However, the division at 300 days is only an approximate one, as we do not know whether there is any sudden break in periods of high and low inclination Mira variables. A more definite answer to this might be sought in the spectra of variables with periods between, say, 275 and 325 days. Another task is to affirm or disprove the large radial velocities in the 150-200 day period-group by selecting as many variables as possible with periods from the shortest ones up to 225 days and determining their radial velocities. Publication: The Astronomical Journal Pub Date: 1960 DOI: 10.1086/108338 Bibcode: 1960AJ.....65S.495O full text sources ADS |

Problems in Astrometry: Some astrometric problems of galactic structure

. Attention is called to the importance of deriving proper motions of the highest accuracy for 0 stars which do not appear to be members of associations. These stars may he found to he moving with large space velocities, and the determination of the direction of these velocities may give a clue as to the place of origin.