IANIGLA 20881
INSTITUTO ARGENTINO DE NIVOLOGIA, GLACIOLOGIA Y CIENCIAS AMBIENTALES
Unidad Ejecutora - UE
artículos
Título:
Kinematics and velocity ellipsoid of the G giants
Autor/es:
BRANHAM, RICHARD L. JR.
Revista:
REVISTA MEXICANA DE ASTRONOMÃA Y ASTROFÃSICA
Editorial:
UNIV NACIONAL AUTONOMA MEXICO
Referencias:
Lugar: México; Año: 2011 vol. 47 p. 197 - 209
ISSN:
0185-1101
Resumen:
To study the kinematics of the G giant stars (luminosity class III) use is made
of proper motions and parallaxes taken from van Leeuwen?s new reduction of the
Hipparcos catalog. 3,075 stars, of which 658 have radial velocities, were used in
the final study. The solution gives: solar velocity of 16.72 ± 0.41 km s−1; Oort?s
constant?s, in units of km s−1 kpc−1, A = 14.05 ± 3.28 and B = −9.30 ± 2.87,
implying a rotational velocity of 198.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
implying a rotational velocity of 198.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
constant?s, in units of km s−1 kpc−1, A = 14.05 ± 3.28 and B = −9.30 ± 2.87,
implying a rotational velocity of 198.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
implying a rotational velocity of 198.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
.72 ± 0.41 km s−1; Oort?s
constant?s, in units of km s−1 kpc−1, A = 14.05 ± 3.28 and B = −9.30 ± 2.87,
implying a rotational velocity of 198.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
implying a rotational velocity of 198.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
−1 kpc−1, A = 14.05 ± 3.28 and B = −9.30 ± 2.87,
implying a rotational velocity of 198.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
.48 ± 26.95 km s−1 if we take the distance to
the Galactic center as 8.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:.2 ± 1.1 kpc; velocity dispersions, in units of km s−1, of:
x = 51.78 ± 0.55, y = 42.81 ± 0.32, z = 28.45 ± 0.22 with a vertex deviation of
3.88 ± 6.62. A comparison of the velocity dispersions with those given by other
spectral types shows that Parenago?s discontinuity also exists for the giant stars.
spectral types shows that Parenago?s discontinuity also exists for the giant stars.
3.88 ± 6.62. A comparison of the velocity dispersions with those given by other
spectral types shows that Parenago?s discontinuity also exists for the giant stars.
spectral types shows that Parenago?s discontinuity also exists for the giant stars.
x = 51.78 ± 0.55, y = 42.81 ± 0.32, z = 28.45 ± 0.22 with a vertex deviation of
3.88 ± 6.62. A comparison of the velocity dispersions with those given by other
spectral types shows that Parenago?s discontinuity also exists for the giant stars.
spectral types shows that Parenago?s discontinuity also exists for the giant stars.
.88 ± 6.62. A comparison of the velocity dispersions with those given by other
spectral types shows that Parenago?s discontinuity also exists for the giant stars.
