Distance determination for RAVE stars using stellar models
... ated. The right panel Fig. 1 shows isochrones of similar chemical composition and can be compared to the stellar tracks shown on the left panel. All stars on the 0.01 Gyr isochrone are still on the main sequence. For older isochrones we can clearly see the main sequence turnoff points, the point at ...
... ated. The right panel Fig. 1 shows isochrones of similar chemical composition and can be compared to the stellar tracks shown on the left panel. All stars on the 0.01 Gyr isochrone are still on the main sequence. For older isochrones we can clearly see the main sequence turnoff points, the point at ...
Lecture 12: Evolution of the Galaxy
... momentum. This results in (a) an accretion disk around equator (b) strong bipolar magnetic field and hence mass loss in bipolar outflow through poles (observed through strong millimetre wave emission in lines of CO) • Typical mass loss rate of protostar ~ 10-4 to 10-6 M⊙/yr • Protostars are often en ...
... momentum. This results in (a) an accretion disk around equator (b) strong bipolar magnetic field and hence mass loss in bipolar outflow through poles (observed through strong millimetre wave emission in lines of CO) • Typical mass loss rate of protostar ~ 10-4 to 10-6 M⊙/yr • Protostars are often en ...
Unit 2―The Stars and Their Diurnal Motion
... 8. The Stars. From the very beginning of a study in astronomy, and as frequently as possible, students should practice watching the stars by night, to become acquainted with the constellations and their movements. To get started in your night time viewing, you should have printed out the maps and ch ...
... 8. The Stars. From the very beginning of a study in astronomy, and as frequently as possible, students should practice watching the stars by night, to become acquainted with the constellations and their movements. To get started in your night time viewing, you should have printed out the maps and ch ...
hr diagrams of star clusters
... isochrone plotted on your HR diagram near the plot of your cluster stars. A small window for setting the Isochrone Parameters will open nearby, with two sliders labeled Age and Adjust (B-V), as well as a choice window labeled Metallicity. By moving the Age and Adjust (B-V) sliders you should be able ...
... isochrone plotted on your HR diagram near the plot of your cluster stars. A small window for setting the Isochrone Parameters will open nearby, with two sliders labeled Age and Adjust (B-V), as well as a choice window labeled Metallicity. By moving the Age and Adjust (B-V) sliders you should be able ...
THE PERIOD OF ROTATION OF THE SUN
... isochrone plotted on your HR diagram near the plot of your cluster stars. A small window for setting the Isochrone Parameters will open nearby, with two sliders labeled Age and Adjust (B-V), as well as a choice window labeled Metallicity. By moving the Age and Adjust (B-V) sliders you should be able ...
... isochrone plotted on your HR diagram near the plot of your cluster stars. A small window for setting the Isochrone Parameters will open nearby, with two sliders labeled Age and Adjust (B-V), as well as a choice window labeled Metallicity. By moving the Age and Adjust (B-V) sliders you should be able ...
A search for a new class of pulsating DA white dwarf stars in the DB
... In that context, Fontaine & Wesemael (1987) explained the DB gap as a natural consequence of the evolution of almost all white dwarfs from planetary nebulae nuclei. They supposed that a slow rise of hydrogen to the surface, as heavier nuclei sink in the strong gravitational field, eventually makes h ...
... In that context, Fontaine & Wesemael (1987) explained the DB gap as a natural consequence of the evolution of almost all white dwarfs from planetary nebulae nuclei. They supposed that a slow rise of hydrogen to the surface, as heavier nuclei sink in the strong gravitational field, eventually makes h ...
PH607lec10-4gal2
... Such a runaway process is called a dynamical instability Note that this process only works if there is enough mass in the disk for the perturbations to modify the gravitational field In early-type spirals (Sa's) where most of the mass is in the bulge not the disk, the instability will be partly supp ...
... Such a runaway process is called a dynamical instability Note that this process only works if there is enough mass in the disk for the perturbations to modify the gravitational field In early-type spirals (Sa's) where most of the mass is in the bulge not the disk, the instability will be partly supp ...
Type II Supernovae
... The trapping of neutrinos was confirmed because the timescale over which the neutrino burst appeared was about 10 seconds and the average detected neutrino energy was about 20 MeV. ...
... The trapping of neutrinos was confirmed because the timescale over which the neutrino burst appeared was about 10 seconds and the average detected neutrino energy was about 20 MeV. ...
Exploring the Universe
... – Distance affects the brightness of stars – What we see is called the apparent magnitude – Absolute magnitude is a measurement of the brightness as if the distance from the earth was 32.6 light years away. A uniform distance, so it’s the real brightness. – Besides the sun, the brightest star is Sir ...
... – Distance affects the brightness of stars – What we see is called the apparent magnitude – Absolute magnitude is a measurement of the brightness as if the distance from the earth was 32.6 light years away. A uniform distance, so it’s the real brightness. – Besides the sun, the brightest star is Sir ...
arXiv:astro-ph/0508448v1 22 Aug 2005
... One potential way of getting around this is to invoke a population with very uneven mass ratios, such that the less massive star still has most of its O star lifetime left after the SN of its companion. However, in order to be an O star on the main sequence at solar metallicity a mass of at least 17 ...
... One potential way of getting around this is to invoke a population with very uneven mass ratios, such that the less massive star still has most of its O star lifetime left after the SN of its companion. However, in order to be an O star on the main sequence at solar metallicity a mass of at least 17 ...
Riccioli Measures the Stars: Observations of the
... measurements of star sizes, including those of Tycho Brahe, that put the observed diameter of first magnitude stars at a minute (60‟‟) or greater, but who then adds that through the telescope star diameters appear much smaller. Riccioli states that the telescope, in “exposing the disks of the stars ...
... measurements of star sizes, including those of Tycho Brahe, that put the observed diameter of first magnitude stars at a minute (60‟‟) or greater, but who then adds that through the telescope star diameters appear much smaller. Riccioli states that the telescope, in “exposing the disks of the stars ...
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.