SPECTRAL ANALYSIS OF A NEWLY DISCOVERED HgMn STAR
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
Chapter 11
... a. About 40 weeks. b. About 30,000 years. c. About 30 million years. d. About 1 billion years. e. About 5 billion years. ...
... a. About 40 weeks. b. About 30,000 years. c. About 30 million years. d. About 1 billion years. e. About 5 billion years. ...
Presentation
... Prialnik, Dina (2000). An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University Press. Stahler, S. W. & Palla, F. (2004). The Formation of Stars. Weinheim: Wiley-VCH. ...
... Prialnik, Dina (2000). An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University Press. Stahler, S. W. & Palla, F. (2004). The Formation of Stars. Weinheim: Wiley-VCH. ...
Mark Rubin
... • At least a fraction of Type IIn supernovae (SNe IIn) are energetic PISNe, providing the only observable examples of this process. They have potential to yield enormous insight into the behavior of high-mass (> 140 Msolar) Pop III stars. • Moreover, SNe IIn are the most luminous SN type in the rest ...
... • At least a fraction of Type IIn supernovae (SNe IIn) are energetic PISNe, providing the only observable examples of this process. They have potential to yield enormous insight into the behavior of high-mass (> 140 Msolar) Pop III stars. • Moreover, SNe IIn are the most luminous SN type in the rest ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... Isochrones are particularly useful for star clusters - all stars born at the same time with the same composition e.g. the Schaller et al. models. Consider stars of different masses but with the same age . Lets make a plot of Log(L/L) vs. LogTeff for an age of 1Gyr. The result is an isochrone. Impor ...
... Isochrones are particularly useful for star clusters - all stars born at the same time with the same composition e.g. the Schaller et al. models. Consider stars of different masses but with the same age . Lets make a plot of Log(L/L) vs. LogTeff for an age of 1Gyr. The result is an isochrone. Impor ...
Practice Questions for Exam 3
... According to the inverse square law of light, how will the apparent brightness of an object change if its distance to us doubles? A. Its apparent brightness will increase by a factor of 4. B. Its apparent brightness will decrease by a factor of 4. C. Its apparent brightness will decrease by a factor ...
... According to the inverse square law of light, how will the apparent brightness of an object change if its distance to us doubles? A. Its apparent brightness will increase by a factor of 4. B. Its apparent brightness will decrease by a factor of 4. C. Its apparent brightness will decrease by a factor ...
Astronomers Find Extremely Large Planet
... Interestingly, these newly discovered silhouette disks are located in several dense clusters composed of hundreds of young forming stars. The fact that the FLAMINGOS survey only found silhouette disks in clusters and not peppered thoughout the immense volume of the molecular clouds supports the poin ...
... Interestingly, these newly discovered silhouette disks are located in several dense clusters composed of hundreds of young forming stars. The fact that the FLAMINGOS survey only found silhouette disks in clusters and not peppered thoughout the immense volume of the molecular clouds supports the poin ...
Oct 06, 2001
... C) It is a shell of gas ejected from a star late in its life. D) It is what is left when a white dwarf star explodes as a supernova. 8) What makes a high-mass star's core collapse? A) Energy from its outer layers compresses its core. B) The only thing that can make a star's core collapse is a collis ...
... C) It is a shell of gas ejected from a star late in its life. D) It is what is left when a white dwarf star explodes as a supernova. 8) What makes a high-mass star's core collapse? A) Energy from its outer layers compresses its core. B) The only thing that can make a star's core collapse is a collis ...
1/20/09 301 Physics Chapter 12 The Family of Stars Triangulation
... • Width of absorption line depends on density: wide for high density, narrow for low density ...
... • Width of absorption line depends on density: wide for high density, narrow for low density ...
Spying into the lives of the stars
... 2 important things about your topic:___________________________ ...
... 2 important things about your topic:___________________________ ...
star signs - Museum of the Rockies
... Celestial Equator. RA is measured in hours, with each hour divided into 60 minutes, and there are 24 hours of RA corresponding to the 24 hours of the day. If you go outside at 10:00pm, choose a bright star near the horizon, and make a note of a landmark on your horizon that it appears above, you wil ...
... Celestial Equator. RA is measured in hours, with each hour divided into 60 minutes, and there are 24 hours of RA corresponding to the 24 hours of the day. If you go outside at 10:00pm, choose a bright star near the horizon, and make a note of a landmark on your horizon that it appears above, you wil ...
P10263v1.2 Lab 6 Text
... When finding the distance to the Pleiades cluster, we used the spectral type information for individual stars in the cluster. That information translated into an estimate of the absolute luminosity. Combined with the measured apparent luminosity and an estimate of “X”, we were able to find the dista ...
... When finding the distance to the Pleiades cluster, we used the spectral type information for individual stars in the cluster. That information translated into an estimate of the absolute luminosity. Combined with the measured apparent luminosity and an estimate of “X”, we were able to find the dista ...
May 2010 - Pomona Valley Amateur Astronomers
... Western University of Health Sciences by day and amateur astronomer by night. We learned of the characteristics of meteor craters, a fairly new science dating only to the start of the 1900s when Daniel Barringer bought land around the crater to be named for him. His searches for a huge iron impactor ...
... Western University of Health Sciences by day and amateur astronomer by night. We learned of the characteristics of meteor craters, a fairly new science dating only to the start of the 1900s when Daniel Barringer bought land around the crater to be named for him. His searches for a huge iron impactor ...
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.