Lecture 12
... Stars: basic observations Basic properties of stars we would like to know in order to compare theory against observations: • Stellar mass M • Stellar radius R • Surface temperature - effective temperature Te • Bolometric luminosity L Recall definition of effective temperature: ...
... Stars: basic observations Basic properties of stars we would like to know in order to compare theory against observations: • Stellar mass M • Stellar radius R • Surface temperature - effective temperature Te • Bolometric luminosity L Recall definition of effective temperature: ...
Age Distributions of Low Mass Stars in the Rho Ophiucus Molecular
... 06s and declination of –24d 32.5s [1]. This makes it accessible from both hemispheres. It consists of two main regions of dense gas and dust. The largest and densest, L1688, is the focus of this work. The Rho Oph complex is located at the eastern edge of the Scorpius-Centaurus OB association in the ...
... 06s and declination of –24d 32.5s [1]. This makes it accessible from both hemispheres. It consists of two main regions of dense gas and dust. The largest and densest, L1688, is the focus of this work. The Rho Oph complex is located at the eastern edge of the Scorpius-Centaurus OB association in the ...
bright - TutorPlus
... depending on their position on the H-R diagram. • Most stars line up along a slightly curved diagonal line called the main sequence. Our Sun is located on the main sequence. • On the main sequence, low mass stars tend to be cooler and less bright whereas high mass stars are hotter, brighter and loca ...
... depending on their position on the H-R diagram. • Most stars line up along a slightly curved diagonal line called the main sequence. Our Sun is located on the main sequence. • On the main sequence, low mass stars tend to be cooler and less bright whereas high mass stars are hotter, brighter and loca ...
the interstellar medium - Howard University Physics and Astronomy
... • Hydrogen constitutes about 90% of all the atoms in the Sun and in newly forming stars. • Helium is the next most abundant (about 9%); all heaver elements constitute about 1% (by number of atoms). • The Sun’s original supply of hydrogen is sufficient to supply its energy output for 10 billion years ...
... • Hydrogen constitutes about 90% of all the atoms in the Sun and in newly forming stars. • Helium is the next most abundant (about 9%); all heaver elements constitute about 1% (by number of atoms). • The Sun’s original supply of hydrogen is sufficient to supply its energy output for 10 billion years ...
Stellar Evolution
... Evolution of Stars More Massive than the Sun Star of more than 8 solar masses can fuse elements far beyond carbon in its core Leads to a very different fate Path across the H-R diagram is essentially a straight line Stays at just about the same luminosity as it cools off Eventually the star dies in ...
... Evolution of Stars More Massive than the Sun Star of more than 8 solar masses can fuse elements far beyond carbon in its core Leads to a very different fate Path across the H-R diagram is essentially a straight line Stays at just about the same luminosity as it cools off Eventually the star dies in ...
AST 1002
... Compare the various theories of stellar evolution and describe how they depend on stellar mass. Compare the various theories explaining the formation of the solar system and our Moon, and justify why the solar nebula theory currently provide the best match of the ...
... Compare the various theories of stellar evolution and describe how they depend on stellar mass. Compare the various theories explaining the formation of the solar system and our Moon, and justify why the solar nebula theory currently provide the best match of the ...
ppt - Wladimir Lyra
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
Pulsars - Chabot College
... accidentally discovered a pulsing radio source Sharp pulse every 1.3 sec. ~1000 light years away Called it a “pulsar”, but what was it? ...
... accidentally discovered a pulsing radio source Sharp pulse every 1.3 sec. ~1000 light years away Called it a “pulsar”, but what was it? ...
Galaxy Formation and Evolution Open Problems
... • Do galaxies, such as the Milky Way, form from accumulation of many smaller systems which have already initiated star formation? • Does star formation begin in a gravitational potential well in which much of the gas is already accumulated? • What is the nature and composition of matter in the galac ...
... • Do galaxies, such as the Milky Way, form from accumulation of many smaller systems which have already initiated star formation? • Does star formation begin in a gravitational potential well in which much of the gas is already accumulated? • What is the nature and composition of matter in the galac ...
The high density QCD phase transition in compact stars
... reverses the infall and ejects the stellar envelope leaving behind a protoneutron star from T.Janka, Nature Phys. 2005 ...
... reverses the infall and ejects the stellar envelope leaving behind a protoneutron star from T.Janka, Nature Phys. 2005 ...
Can you write numbers in scientific notation
... What determines what object will be left behind after a star dies out? What are the properties of each of those objects? How does Einstein’s model of gravity differ from Newton’s description? Why Einstein’s description taken to be “more complete” than Newton’s? What are the effects an outside obser ...
... What determines what object will be left behind after a star dies out? What are the properties of each of those objects? How does Einstein’s model of gravity differ from Newton’s description? Why Einstein’s description taken to be “more complete” than Newton’s? What are the effects an outside obser ...
Distances farther out
... Giant stars have spread about average --- , If 39 Cnc is as bright as Uma (ie Mv = -0.3), then it would be 50 % farther away. In a cluster can use several stars or whole main sequence to increase precision. Only need from before, M of various stars, ie need to calibrate HR diagram and various lumi ...
... Giant stars have spread about average --- , If 39 Cnc is as bright as Uma (ie Mv = -0.3), then it would be 50 % farther away. In a cluster can use several stars or whole main sequence to increase precision. Only need from before, M of various stars, ie need to calibrate HR diagram and various lumi ...
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.