Notes for Class 7, March 2
... • We are finding other stars with planets o Present techniques best for planets close to star o So far, too close to star, too hot o If planets around other stars are common, maybe there will be some planets with the right conditions, and maybe some of them will have life ...
... • We are finding other stars with planets o Present techniques best for planets close to star o So far, too close to star, too hot o If planets around other stars are common, maybe there will be some planets with the right conditions, and maybe some of them will have life ...
fundamental properties of kepler planet- candidate
... done using a median filter with a length chosen according to the measured duration of the transit. In an alternative approach, all transits were phase-clipped from the time series using the periods and epochs listed in Batalha et al. (2013). Note that for typical transit durations and periods, the i ...
... done using a median filter with a length chosen according to the measured duration of the transit. In an alternative approach, all transits were phase-clipped from the time series using the periods and epochs listed in Batalha et al. (2013). Note that for typical transit durations and periods, the i ...
Theory of cooling neutron stars versus observations
... can be solved by comparing theoretical models with observations of neutron stars. The attempts to solve this long-standing problem by different methods are numerous (e.g., Refs. [1, 2]). Here we discuss current results obtained from studies of cooling isolated neutron stars. The first papers on neut ...
... can be solved by comparing theoretical models with observations of neutron stars. The attempts to solve this long-standing problem by different methods are numerous (e.g., Refs. [1, 2]). Here we discuss current results obtained from studies of cooling isolated neutron stars. The first papers on neut ...
File
... That's right—it gets bigger (more massive) which means more gravity and more particles are attracted and so on..... So the “ball” of gas and dust eventually gets so big its center gets very compacted. ...
... That's right—it gets bigger (more massive) which means more gravity and more particles are attracted and so on..... So the “ball” of gas and dust eventually gets so big its center gets very compacted. ...
Symbiotic Stars as Laboratories for the Study of
... Abstract Symbiotic binary stars typically consist of a white dwarf (WD) that accretes material from the wind of a companion red giant. Orbital periods for these binaries are on the order of years, and their relatively small optical outbursts tend to occur every few years to decades. In some symbioti ...
... Abstract Symbiotic binary stars typically consist of a white dwarf (WD) that accretes material from the wind of a companion red giant. Orbital periods for these binaries are on the order of years, and their relatively small optical outbursts tend to occur every few years to decades. In some symbioti ...
Galaxies and Active Galaxies
... – Very luminous galaxies tend to be either the elliptical or spiral type, so they are the ones often displayed in astronomy textbooks. ...
... – Very luminous galaxies tend to be either the elliptical or spiral type, so they are the ones often displayed in astronomy textbooks. ...
– 1 – 1. Emission Lines in Nearby Galaxies 1.1.
... ratio of their strengths will yields a measure of temperature. The key diagnostic lines used include 4363 Å of [OIII], but this line is often too weak to be observed. Note that these are all forbidden lines, which means they have low transition probabilities. When the 4363 Å line is too weak to be ...
... ratio of their strengths will yields a measure of temperature. The key diagnostic lines used include 4363 Å of [OIII], but this line is often too weak to be observed. Note that these are all forbidden lines, which means they have low transition probabilities. When the 4363 Å line is too weak to be ...
Variable stars in the globular cluster M 92
... Kadla et al. (1983). They also give the cross-identification of variable stars in the third catalogue of Sawyer-Hogg (1973) with numbering system of Nassau (1938). It appears now that v12 is Nassau’s star no. 10 and v15 corresponds to Nassau’s star no. 12. Oosterhoff (1944) rediscussed the observati ...
... Kadla et al. (1983). They also give the cross-identification of variable stars in the third catalogue of Sawyer-Hogg (1973) with numbering system of Nassau (1938). It appears now that v12 is Nassau’s star no. 10 and v15 corresponds to Nassau’s star no. 12. Oosterhoff (1944) rediscussed the observati ...
Galaxy Evolution
... (for example, they have stopped following the cosmic expansion). The theory of gravitational instability predicts that the number of virialized systems that have formed at any given time depends on their mass, with more massive systems being less abundant than less massive ones. It also predicts tha ...
... (for example, they have stopped following the cosmic expansion). The theory of gravitational instability predicts that the number of virialized systems that have formed at any given time depends on their mass, with more massive systems being less abundant than less massive ones. It also predicts tha ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... (for example, they have stopped following the cosmic expansion). The theory of gravitational instability predicts that the number of virialized systems that have formed at any given time depends on their mass, with more massive systems being less abundant than less massive ones. It also predicts tha ...
... (for example, they have stopped following the cosmic expansion). The theory of gravitational instability predicts that the number of virialized systems that have formed at any given time depends on their mass, with more massive systems being less abundant than less massive ones. It also predicts tha ...
Galaxies
... primordial—dating from the very early days of the Universe. There is not nearly enough of it to account for most of the matter in galaxy clusters. ...
... primordial—dating from the very early days of the Universe. There is not nearly enough of it to account for most of the matter in galaxy clusters. ...
High mass-to-light ratios of UCDs
... elevated mass-to-light ratios of the nuclear star clusters. ❒ Later tidal stripping leaves only the nuclear star cluster behind which becomes a UCD. ❒ Dark matter might therefore be another way to explain the high massto-light ratios of UCDs. =⇒ Since a similar formation scenario is discussed for a ...
... elevated mass-to-light ratios of the nuclear star clusters. ❒ Later tidal stripping leaves only the nuclear star cluster behind which becomes a UCD. ❒ Dark matter might therefore be another way to explain the high massto-light ratios of UCDs. =⇒ Since a similar formation scenario is discussed for a ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.