Astronomy Laboratory Manual
... There's only one way to get to know a map like this. Hold it out in front of you as you face the horizon. Twist it around so the map edge labeled with the direction you're facing is down. The correct horizon on the map will now appear horizontal and match the horizon in front of you. Now you can com ...
... There's only one way to get to know a map like this. Hold it out in front of you as you face the horizon. Twist it around so the map edge labeled with the direction you're facing is down. The correct horizon on the map will now appear horizontal and match the horizon in front of you. Now you can com ...
Lokal fulltext - Chalmers Publication Library
... in 1984 at Vega (α Lyrae, spectral class A0 V) by Aumann et al. (1984) with IRAS (Infrared Astronomical Satellite). However, as they saw the dust emission only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpre ...
... in 1984 at Vega (α Lyrae, spectral class A0 V) by Aumann et al. (1984) with IRAS (Infrared Astronomical Satellite). However, as they saw the dust emission only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpre ...
SGR 1900+14
... GRB prompt emission peak fluxes: 10-8-10-3 ergs/cm2 s X-ray afterglows of long bursts: ~10-11 – 10-13 ergs/cm2 s Previous giant flares: ~10-3 ergs/cm2 s Typical SGR bursts: 10-9 – 10-6 ergs/cm2 s ...
... GRB prompt emission peak fluxes: 10-8-10-3 ergs/cm2 s X-ray afterglows of long bursts: ~10-11 – 10-13 ergs/cm2 s Previous giant flares: ~10-3 ergs/cm2 s Typical SGR bursts: 10-9 – 10-6 ergs/cm2 s ...
The evolution of spiral galaxies in clusters Kutdemir, Elif
... Evidence have been accumulating, mainly from HI studies, on the importance of cold gas accretion in the local universe: A large number of galaxies are accompanied by gas-rich dwarfs or are surrounded by HI cloud complexes, tails and filaments (Sancisi et al. 2008). Most of the high-velocity clouds a ...
... Evidence have been accumulating, mainly from HI studies, on the importance of cold gas accretion in the local universe: A large number of galaxies are accompanied by gas-rich dwarfs or are surrounded by HI cloud complexes, tails and filaments (Sancisi et al. 2008). Most of the high-velocity clouds a ...
Baryons at Low Densities: The Stellar Halos around Galaxies
... clusters) survey. The high angular resolution of the Hubble Space Telescope (HST) allows the detection of single stars in halos at larger distances and in denser regions — hence investigating the transition regions between the disc and halo. All MW-like galaxies observed by GHOSTS have extended stel ...
... clusters) survey. The high angular resolution of the Hubble Space Telescope (HST) allows the detection of single stars in halos at larger distances and in denser regions — hence investigating the transition regions between the disc and halo. All MW-like galaxies observed by GHOSTS have extended stel ...
Astrometric accuracy during the past 2000 years
... have used this comparison to derive below that the errors given in the FK5 of positions at the mean epoch and of the proper motions should be multiplied by a factor about 1.6 to obtain external errors. For any other historical catalogue it would be sufficient to take a representative sample of less ...
... have used this comparison to derive below that the errors given in the FK5 of positions at the mean epoch and of the proper motions should be multiplied by a factor about 1.6 to obtain external errors. For any other historical catalogue it would be sufficient to take a representative sample of less ...
Evolution of low mass stars
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
Introduction
... some exoplanets. With the latter, polar or retrograde planet orbits can be identified. However, as the inclinations are degenerate over the inclination to the plane of the sky, it is not possible to compare them to the values in the Solar System or in the planet formation and evolution models. So fa ...
... some exoplanets. With the latter, polar or retrograde planet orbits can be identified. However, as the inclinations are degenerate over the inclination to the plane of the sky, it is not possible to compare them to the values in the Solar System or in the planet formation and evolution models. So fa ...
Unlocking the secrets of stellar haloes using combined star counts
... observations, a small fraction – the EBL – comes from behind. Provided that the existing direct measurements of the optical EBL are correct (Bernstein 2007), most of this light appears to be diffuse (i.e. unresolved with all existing instruments). Unlike the other components of the night sky flux, t ...
... observations, a small fraction – the EBL – comes from behind. Provided that the existing direct measurements of the optical EBL are correct (Bernstein 2007), most of this light appears to be diffuse (i.e. unresolved with all existing instruments). Unlike the other components of the night sky flux, t ...
Ages of Young Stars
... of (undepleted) Li in a low-mass star at a known distance and luminosity, or less accurately with an estimated Teff , will give an upper limit to its age. Conversely, the lack of Li in a similar star places a lower limit to its age. This can be useful for finding low-mass members of nearby, young mo ...
... of (undepleted) Li in a low-mass star at a known distance and luminosity, or less accurately with an estimated Teff , will give an upper limit to its age. Conversely, the lack of Li in a similar star places a lower limit to its age. This can be useful for finding low-mass members of nearby, young mo ...
Ages of young stars
... are combinations of theoretical uncertainties and observational uncertainties associated with estimating the luminosity of the LDB. Contributing to the latter are distance estimates, reddening and bolometric corrections (for stellar luminosity not in the band observed), but these are usually small c ...
... are combinations of theoretical uncertainties and observational uncertainties associated with estimating the luminosity of the LDB. Contributing to the latter are distance estimates, reddening and bolometric corrections (for stellar luminosity not in the band observed), but these are usually small c ...
ALMA - ESO
... Most of the radiation emitted by stars is absorbed by dust and re-radiated in the 3 micrometer to 1 mm wavelength range The luminous IR galaxies trace regions where the concentration of galaxies is largest, and trace the formation of large scale structures. ...
... Most of the radiation emitted by stars is absorbed by dust and re-radiated in the 3 micrometer to 1 mm wavelength range The luminous IR galaxies trace regions where the concentration of galaxies is largest, and trace the formation of large scale structures. ...
The old globular cluster system of the dIrr galaxy NGC 1427A in the
... (2000) and Harris (2003). In all these models, the GCSs of low-mass dwarf galaxies, the most numerous galaxy type in galaxy clusters (Sandage 2005, and references therein), are envisioned as the building blocks of the GCSs of the more massive galaxies. At present the role of the GCSs of dIrr galaxie ...
... (2000) and Harris (2003). In all these models, the GCSs of low-mass dwarf galaxies, the most numerous galaxy type in galaxy clusters (Sandage 2005, and references therein), are envisioned as the building blocks of the GCSs of the more massive galaxies. At present the role of the GCSs of dIrr galaxie ...
The Sun
... more complex it seems, and the less astronomers seem to know about it. • It pays to look at this paradox from another direction. – The sun is an average star, and there are billions like it in the sky. – The more astronomers can learn from the convenient example of the sun, the more they will know a ...
... more complex it seems, and the less astronomers seem to know about it. • It pays to look at this paradox from another direction. – The sun is an average star, and there are billions like it in the sky. – The more astronomers can learn from the convenient example of the sun, the more they will know a ...
Open clusters and associations in the Gaia era
... Another difference between a cluster and an association arising directly from their definition is the lifetime. An open cluster is loosely bound and its star members will stay together for about 100 Myr to a few Gyr for the densest ones, before it gets disrupted by the galactic tidal field. On the c ...
... Another difference between a cluster and an association arising directly from their definition is the lifetime. An open cluster is loosely bound and its star members will stay together for about 100 Myr to a few Gyr for the densest ones, before it gets disrupted by the galactic tidal field. On the c ...
Stars Evolution of High Mass Stars Nucleosynthesis Supernovae
... © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
... © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
Teil 2
... particular field lines. Whether such magnetic coupling in tidally locked stars has an impact on the dynamo and the formation and rise of flux tubes remains to be determined but is suggested from the current results. As a by-product of the Doppler-imaging analysis, we obtained one of the most precise ...
... particular field lines. Whether such magnetic coupling in tidally locked stars has an impact on the dynamo and the formation and rise of flux tubes remains to be determined but is suggested from the current results. As a by-product of the Doppler-imaging analysis, we obtained one of the most precise ...
Ursa Minor
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.