Angular Momentum Evolution of Young Low
... the best way to trace their angular momentum evolution from about 1 million years ago (Ma) to 1 billion years ago (Ga). This section discusses the observational studies of stellar rotation performed since the PPV review by Herbst al. (2007), for solar-type stars and lower-mass stars, down to the bro ...
... the best way to trace their angular momentum evolution from about 1 million years ago (Ma) to 1 billion years ago (Ga). This section discusses the observational studies of stellar rotation performed since the PPV review by Herbst al. (2007), for solar-type stars and lower-mass stars, down to the bro ...
The Halo of the Milky Way
... are plots through the data in Fig. 8. A parabola with minimum at l = 155◦ has been drawn over the second panel. The star counts on the right half of the plots show the stars from the Sgr dwarf tidal stream. The top panel, which gives the densities of spheroid stars with the largest distances from th ...
... are plots through the data in Fig. 8. A parabola with minimum at l = 155◦ has been drawn over the second panel. The star counts on the right half of the plots show the stars from the Sgr dwarf tidal stream. The top panel, which gives the densities of spheroid stars with the largest distances from th ...
Chapter 16--Properties of Stars
... detector, such as a CCD, that records how much energy strikes its light-sensitive surface each second. For example, such a detector would record an apparent brightness of 2.7 108 watt per square meter from Alpha Centauri A. The only difficulties involved in measuring apparent brightness are makin ...
... detector, such as a CCD, that records how much energy strikes its light-sensitive surface each second. For example, such a detector would record an apparent brightness of 2.7 108 watt per square meter from Alpha Centauri A. The only difficulties involved in measuring apparent brightness are makin ...
Part IV: Stars
... by comparing their predictions for the radius, surface temperature, and luminosity, as well as other observable parameters generated by studying helioseismology. Helioseismology allows us to probe the conditions in the solar interior. The models make testable predictions that allow us to explain the ...
... by comparing their predictions for the radius, surface temperature, and luminosity, as well as other observable parameters generated by studying helioseismology. Helioseismology allows us to probe the conditions in the solar interior. The models make testable predictions that allow us to explain the ...
Article PDF - IOPscience
... M31. They span distances in the range of ∼45 arcmin (G76) to ∼4 deg (B514) from the center of M31, thus allowing us to probe different areas of Andromeda, from the galaxy’s unperturbed halo to regions close to the giant stream. We are aware that these few clusters may not necessarily be representati ...
... M31. They span distances in the range of ∼45 arcmin (G76) to ∼4 deg (B514) from the center of M31, thus allowing us to probe different areas of Andromeda, from the galaxy’s unperturbed halo to regions close to the giant stream. We are aware that these few clusters may not necessarily be representati ...
103-122
... example, the rms scatter of the [Fe/H] values from about 20 Fe I lines is only 0.05 dex for a typical star—all values fall within ±0.10 dex of the mean. The light elements available are Na, Mg, Al, Si, and Ca. Titanium which behaves much like an α-element was also included along with Ni, and the hea ...
... example, the rms scatter of the [Fe/H] values from about 20 Fe I lines is only 0.05 dex for a typical star—all values fall within ±0.10 dex of the mean. The light elements available are Na, Mg, Al, Si, and Ca. Titanium which behaves much like an α-element was also included along with Ni, and the hea ...
fred`s 2017 astronomy challenge
... difficult to find easily unless you know where to look. Give is a few million years, and it will be a lot easier to see. Follow down from Cassiopeia into the constellation of Andromeda it ...
... difficult to find easily unless you know where to look. Give is a few million years, and it will be a lot easier to see. Follow down from Cassiopeia into the constellation of Andromeda it ...
Llama_2015_AJ_Transiting - St Andrews Research Repository
... may in principle be possible to use transits at these wavelengths to study the properties of the corona. The duration of transit events at these wavelengths may be longer than the corresponding optical events which are only sensitive to light from the photosphere of the star. In our simulated 94–335 ...
... may in principle be possible to use transits at these wavelengths to study the properties of the corona. The duration of transit events at these wavelengths may be longer than the corresponding optical events which are only sensitive to light from the photosphere of the star. In our simulated 94–335 ...
Here - Astrophysics Research Institute
... Converting to Alt-Az Coordinates Given: the latitude of the observer, Φ, the hour angle, HA and Declination, δ we can calculate azimuth A and altitude a. By the cosine rule: cos(90°-a) = cos(90°-δ) cos(90°-Φ) + sin(90°-δ) sin(90°-Φ) cos(HA) which simplifies to: sin(a) = sin(δ) sin(Φ) + cos(δ) cos(Φ ...
... Converting to Alt-Az Coordinates Given: the latitude of the observer, Φ, the hour angle, HA and Declination, δ we can calculate azimuth A and altitude a. By the cosine rule: cos(90°-a) = cos(90°-δ) cos(90°-Φ) + sin(90°-δ) sin(90°-Φ) cos(HA) which simplifies to: sin(a) = sin(δ) sin(Φ) + cos(δ) cos(Φ ...
Anatomy of a Supernova - hrsbstaff.ednet.ns.ca
... op computer models that start with nuclear physics and pretime to expand. But tbis model also had problems. Some Type dict observed ligbt curves and spectra. la's eject elements like calcium at nearly one-tenth the speed Fortunately, astronomers have a starting point. Mathematiof light. It was hard ...
... op computer models that start with nuclear physics and pretime to expand. But tbis model also had problems. Some Type dict observed ligbt curves and spectra. la's eject elements like calcium at nearly one-tenth the speed Fortunately, astronomers have a starting point. Mathematiof light. It was hard ...
... change? Well, this increase is primarily due to the humanmade greenhouse gases. Levels of CO2 have increased from around 280 parts per million (ppm) to around 380 ppm now. Studies of ice core show that concentrations of CO2 have not been so high for nearly half a million years. At the current rate o ...
Properties of simulated galaxies at z~4-7
... Extension to lower redshift to test further the interplay between galactic winds & AGN feedback. LAEs at z ~ 3: ANGUS + CRASHα, in collaboration with Akila Jeeson-Daniel (UoM). ...
... Extension to lower redshift to test further the interplay between galactic winds & AGN feedback. LAEs at z ~ 3: ANGUS + CRASHα, in collaboration with Akila Jeeson-Daniel (UoM). ...
Starburst Galaxies Under the Microscope: High
... 10.5 µm [S IV] line, an ionisation stage requiring 34.8 eV (while the 12.8 µm [Ne II] line requires only 21.6 eV); in particular in cluster 2 the [S IV]/[Ne II] ratio in our data is higher than in larger aperture Spitzer data, significantly affecting the interpretation of the results, and indicating ...
... 10.5 µm [S IV] line, an ionisation stage requiring 34.8 eV (while the 12.8 µm [Ne II] line requires only 21.6 eV); in particular in cluster 2 the [S IV]/[Ne II] ratio in our data is higher than in larger aperture Spitzer data, significantly affecting the interpretation of the results, and indicating ...
Impact of atmospheric refraction: How deeply can we probe exo
... papers (Garcı́a Muñoz & Mills 2012; Garcı́a Muñoz et al. 2012; Bétrémieux & Kaltenegger 2013; Rodler & López-Morales 2014; Misra et al. 2014). At the top of the atmosphere, the ray from the star is undeflected. As the impact parameter of the rays decreases, the deflection of the rays increases. ...
... papers (Garcı́a Muñoz & Mills 2012; Garcı́a Muñoz et al. 2012; Bétrémieux & Kaltenegger 2013; Rodler & López-Morales 2014; Misra et al. 2014). At the top of the atmosphere, the ray from the star is undeflected. As the impact parameter of the rays decreases, the deflection of the rays increases. ...
NSDL/NSTA Web Seminar: Celebrating Astronomy: A Star`s Story
... We think Low mass (< 1 Msun) stars also puff out, and eventually become white dwarfs. We do know they are very long lived -- longer than the universe is old. ...
... We think Low mass (< 1 Msun) stars also puff out, and eventually become white dwarfs. We do know they are very long lived -- longer than the universe is old. ...
Celebrating Astronomy: The Life of a Star
... We think Low mass (< 1 Msun) stars also puff out, and eventually become white dwarfs. We do know they are very long lived -- longer than the universe is old. ...
... We think Low mass (< 1 Msun) stars also puff out, and eventually become white dwarfs. We do know they are very long lived -- longer than the universe is old. ...
Astronomical Techniques Course
... 7.) Determine the value of airmass for a star with RA: 10h:30m:15s and Dec: 30deg: 15‟:15‟‟. Observations are from IAO, Hanle on 21 Feb 2007 at 8:00PM (IST). 8.) For a star in certain direction the colour excess E(B-V) is found out to be 1.0. Given the measured magnitudes of Vmag = 8.0 and Bmag = 10 ...
... 7.) Determine the value of airmass for a star with RA: 10h:30m:15s and Dec: 30deg: 15‟:15‟‟. Observations are from IAO, Hanle on 21 Feb 2007 at 8:00PM (IST). 8.) For a star in certain direction the colour excess E(B-V) is found out to be 1.0. Given the measured magnitudes of Vmag = 8.0 and Bmag = 10 ...
The self-enrichment of galactic halo globular clusters: a clue to their
... mass stars, easier to eject than the heavier ones. Our scenario requires that a significant fraction of the field stars now observed in the halo have been evaporated from globular clusters at an earlier epoch. Indeed, Johnston et al. (1999) claim that GC destruction processes are rather efficient : ...
... mass stars, easier to eject than the heavier ones. Our scenario requires that a significant fraction of the field stars now observed in the halo have been evaporated from globular clusters at an earlier epoch. Indeed, Johnston et al. (1999) claim that GC destruction processes are rather efficient : ...
5. cosmic distance ladder ii: standard candles
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
Characteristics of Our Galaxy
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
Learning Objectives
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
AST1100 Lecture Notes
... Several stars show periodic changes in their apparent magnitudes. This was first thought to be caused by dark spots on a rotating star’s surface: When the dark spots were turned towards us, the star appeared fainter, when the spots were turned away from us, the star appeared brighter. Today we know ...
... Several stars show periodic changes in their apparent magnitudes. This was first thought to be caused by dark spots on a rotating star’s surface: When the dark spots were turned towards us, the star appeared fainter, when the spots were turned away from us, the star appeared brighter. Today we know ...
cranmer_nessc_oct2008
... Angular momentum removal • Many accreting T Tauri stars are slowly rotating, despite the fact that disk accretion adds angular momentum to the star (e.g., ...
... Angular momentum removal • Many accreting T Tauri stars are slowly rotating, despite the fact that disk accretion adds angular momentum to the star (e.g., ...
How I Learned to Stop Worrying and Love Eclipsing Binaries
... ~⅓ of SB1s contain compact remnant companions (Regulus) OGLE EBs in MCs probe low Z, extreme q, and intermediate P Discovered new class of reflecting pre-MS + MS EBs EBs as age indicators: - kinematics of H II regions (feedback) - evolution of eccentricity (tides) Mind your Ps and Qs: at intermediat ...
... ~⅓ of SB1s contain compact remnant companions (Regulus) OGLE EBs in MCs probe low Z, extreme q, and intermediate P Discovered new class of reflecting pre-MS + MS EBs EBs as age indicators: - kinematics of H II regions (feedback) - evolution of eccentricity (tides) Mind your Ps and Qs: at intermediat ...