Next: Binary Radio Pulsars Up: A Tutorial on Radio Previous: Assignment 4 . Binary Radio Pulsars . Millisecond Pulsars . Binary companions and their orbits . X-ray Binaries . Evolution in massive binaries . Evolution in low mass binaries . Eccentricities of pulsar orbits . ... The Masses of Neutron Stars . ... Strong v Weak tests . ... Strong Equivalence Principle: . ... Binary Pulsars . ... Invariance of Lorentz Transformations . ... Conservation Laws, Lorentz Invariance . ...

Next: DIRECT MASSES FOR BXCIR Up: EXTREME HELIUM STARS: PULSATION Previous: PULSATION PROPERTIES . As already indicated, V652Her is an important EHe star because its relatively short pulsation period and large amplitude pulsations allow its overall dimensions to be determined with high precision. ... Saio & Nomoto (1998) made the first successful models for the merger of two carbon-oxygen white dwarfs, and prompted Saio & Jeffery (2000) to attempt models for the merger of two helium white dwarfs. ...

Next: Binary Radiopulsars with Black Up: Black Holes in Binaries Previous: Black Holes in Binaries . Two different types of stellar BH formation exist: (1) direct core collapse   of a massive star and (2) AIC of a NS. A BH of the first type presumably will have a mass comparable to that of the collapsing star and can be born both from a single star and in a binary system. ... Next: Binary Radiopulsars with Black Up: Black Holes in Binaries Previous: Black Holes in Binaries Mike E. Prokhorov . ...

... Since the reddening found for the stars in Table 13 was small, no reddening correction was attempted. ... These diamonds indicate the positions of very low mass, 3 Myr old, objects from the work of Burrows et al. ... This optical V versus R - I scheme is a very powerful method of detecting very low mass (VLM) objects. ... Because of this, young brown dwarfs are intrinsically no more difficult to observe in the optical than low mass stars at the age of Orionis. ...

. Next: Cross indices Up: Derived parameters Previous: Diameters Contents . i_binaries Estimate I from MASS1/2+MF or MASS1/2+M1/2SIN3I. a_binaries Estimate A from MASS1/2+P+D. k_binaries Estimate K1+K2. m_binaries Estimate secondary mass from primary of an SB2 . Christian Hummel 2015-04-28

Next: A candidate young galaxy? Up: Results and discussion Previous: Current star formation rate . The integrated H I line flux, the characteristic widths of 21 cm line profile W 50 and W 20 (for a Hanning smoothing of 10.6 km s -1 ), and the derived H I mass for HS 0822+3542 are presented in Table 1 . The small H I mass 2.4 of this galaxy is consistent with its low optical luminosity. ... A rough estimation can be made also on the dynamical mass of HS 0822+3542. ...

... Abubekerov M.K., Lipunov V.M. "The Lower Temperature Limits Of Accretors" Astronomy Reports, 2003, Vol. 47, Issue 8, pp.679-684. ... Abubekerov M.K., Antokhina E.A., Cherepashchuk A.M. "The Masses of X-ray Pulsars in Binary systems with OB Supergiants" Astronomy Reports, 2004, Vol. ... Abubekerov M.K., Antokhina E.A., Cherepashchuk A.M., Shimanskii V.V. "The Mass of the Compact Object in the Low-Mass X-ray Binary 2S 0921-630" Astronomy Reports Astronomy Reports, 2006, Vol.50, Issue 7, pp.544-552. ...

... Interacting galaxies . ... Catalogues . ... We define a volume limited sample of over 14,000 early-type galaxies (ETGs) selected from data release six of the Sloan Digital Sky Survey. The density of environment of each galaxy is robustly measured. By comparing narrow band spectral line indices with recent models of simple stellar populations (SSPs) we investigate trends in the star formation history as a function of galaxy mass (velocity dispersion), density of environment and galactic radius. ...

... Harald Ebeling, University of Hawaii . ... Abstract . ... Identifying the host galaxies for optically dark gamma-ray bursts . ... The Architecture of Exoplanetary Systems . ... The proposers use Chandra to obtain precise positions of the GRB, and deep follow-up HST observations to search for the host galaxy. ... The calibration of thsi relation rests on observations of binary systems, primarily eclipsing binaries at masses above 1 M Sun , and primarily astrometric binaries at sub-solar masses. ...

... The sample of the Local Volume galaxies (distance smaller than 10 Mpc) gives a unique opportunity to study the properties of galaxies including the weakest objects: the absolute magnitude M B -10 and the virial mass M vir 10 9 M x263C;. ... Luminosity function of the Local Volume galaxies. ... The luminosity functions for galaxies are presented: red dashed line - from the 2dFGRS survey (Norberg et al. 2002); blue dash-dotted line - from the SDSS survey (Blanton et al. ...

... Development of Ideas of Structure and Evolution of Stars. Integral Features of Stars, Which Determine Their Structure, Direction and Rate of Evolutuion. ... Connection between Potential and Thermal Energy of Star. ... Structure of a Main Sequence Star. Features of Massive Stars Evolution on the Main Sequence. Internal Structure of the Sun. ... White Dwarfs, Their Features. ... Evolution from the Main Sequence of Massive Stars. ... Evolution of Small Mass Stars till White Dwarfs Sequence. ...

... In this talk, I will discuss a study of the effect of ionization on the low end of HI mass function. The existence of a large population of low mass galaxies follows from CDM theory. ... HIDEEP found no low HI column density galaxies. One possible explanation is that the disks are "frozen". ... We assume that galaxies are exposed to an ionizing background radiation, from a uniform quasar distribution. ... We find a gap in the average column densities around N H which drops to 10 17 cm -2 . ...

... CXC , NASA Explanation: Large, massive stars end their furious lives in spectacular supernova explosions -- but small, low mass stars may encounter a similar fate. In fact, instead of simply cooling off and quietly fading away, some white dwarf stars in binary star systems are thought to draw enough mass from their companions to become unstable, triggering a nuclear detonation . ... Publications with keywords: supernova remnant - white dwarf - X-ray . ... Vela Supernova Remnant in Visible Light . ...

In the Table below the masses of some asteroids which were determined during the last years are listed. ... The listed values were determined from observations of many test bodies by the weighted least square fit for one perturbing mass and corrections to the orbit elements of all used test bodies. ... based on the observations of 98 asteroids (including 50278) with the values of standard error of mass determination less than 3.0 10 -11 M Sun . ... Mass . ... 3) Mass 121 : 0.74 x 10 -11 M Sun ; . ...

... The relationship of the mass and the observed galactocentric distance R -- (a), and that of the mass and the total dissipation velocity n taken from Gnedin, Ostriker (1997) -- (b). The dotted line in diagram (a) shows the "cone of survival" according to the paper by Surdin and Arkhipova (1998) . ... The solid line is a regression stright line for the main sequence of clusters, and the dotted line parallel to it separates the sequence of clusters of anomalously small mass shown by open triangles. ...

... Editor's choices for the most educational Astronomy Pictures of the Day about binary stars: . APOD: 1999 December 19 – Accretion Disk Binary System . Explanation: Our Sun is unusual in that it is alone - most stars occur in multiple or binary systems . In a binary system, the higher mass star will evolve faster and will eventually become a compact object - either a white dwarf star, a neutron star , or black hole . ... APOD: 2003 November 10 – An Intermediate Polar Binary System . ...

... More on 51 Peg: . The discovery of a Jupiter--mass planet in orbit around the solar--type star 51Peg has been reported by Michel Mayor and Didier Queloz (Geneva Observatory) on October 6th at the 9th Cambridge workshop on "cool stars, stellar systems, and the sun" held at Florence (Italy). ... Recall that the measurements of radial velocity only yield v sin i which in turn gives us M sin i. For most values of i, sin i will be greater than 0.5 and this gives a mass estimate of 0.5 Jupiter masses. ...

Properties of the interstellar gas clouds . ... The angular resolution of this Survey was 2.4' x 130', velocity resolution was 6.3 km/s, r.m.s. fluctuations of antenna temperature (T a ) was 0.25 K. All clouds with kinematical distances r a Some selection effects were discovered and our statistic results were corrected for them. Figure 1. ... In the very high mass range the number of neutral gas clouds may be decreased because of gravitational instability or/and molecularization. ...

Galileo showed convincingly that heavy objects fell no faster that light ones. ... If an iron ball was pulled down with a much greater force than a wooden one of the same size, why didn't it fall any faster? ... 1) It is harder to lift. ... It is the fact that the loaded wagon has a greater mass that gives it a larger inertia , a larger tendency to oppose any change in its state of rest or of constant motion in a straight line. ... One important quantity was the body mass of the astronauts. ...

Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System Characteristics Formation Exosolar Planets Class 3 Stars The S un Stellar Evolution of Low and High Mass Stars Deaths of Stars Exotic Stars Class 4 Galaxies Galaxy Classification Formation of Galaxies Galactic ... Low mass stars live and die differently than high mass stars. ...