
Time From the Perspective of a Particle Physicist
... • acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e n + neutrino • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Star or Black Hole • Most SN are this type PHYS 1 ...
... • acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e n + neutrino • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Star or Black Hole • Most SN are this type PHYS 1 ...
• This chapter concentrates on five goals:
... • Two, in the surface layers of stars hotter than about 20,000 K, there are many violent collisions between atoms. • These excite electrons to high energy levels or knock the electrons completely out of most atoms—so they become ionized. – In this case, few hydrogen atoms will have electrons in the ...
... • Two, in the surface layers of stars hotter than about 20,000 K, there are many violent collisions between atoms. • These excite electrons to high energy levels or knock the electrons completely out of most atoms—so they become ionized. – In this case, few hydrogen atoms will have electrons in the ...
GET WORKSHEETS FROM MY ASSIGNMENTS PAGE Mrs
... 1. What are the stages in a low-mass star’s life? 2. What are the stages in a high-mass star’s life? 3. What determines a star’s type? 4. What makes the Sun an ideal star for life? 5. Is the Sun a low-mass or high-mass star? 6. Looking at the H-R diagram, what are the: hottest, dimmest stars? cooles ...
... 1. What are the stages in a low-mass star’s life? 2. What are the stages in a high-mass star’s life? 3. What determines a star’s type? 4. What makes the Sun an ideal star for life? 5. Is the Sun a low-mass or high-mass star? 6. Looking at the H-R diagram, what are the: hottest, dimmest stars? cooles ...
Nucleosynthesis and the death of stars
... 4 H He + energy + neutrinos Mass of 4 H > Mass of 1 He •In every second, 600 million tons of hydrogen converts into helium to power the Sun •At this rate, the Sun can continue hydrogen fusion for more than 6 billion years. ...
... 4 H He + energy + neutrinos Mass of 4 H > Mass of 1 He •In every second, 600 million tons of hydrogen converts into helium to power the Sun •At this rate, the Sun can continue hydrogen fusion for more than 6 billion years. ...
Powerpoint
... (t = 0 defined by the neutrino burst) – Kirshner et al, ApJ, 320, 602, (1987), showed an emission temperature of 15,000 K that was already declining rapidly. Ultraviolet observations later (Fransson et al, ApJ, 336, 429 (1989) showed narrow emission lines of N III, N IV, N V, and C III (all in the 1 ...
... (t = 0 defined by the neutrino burst) – Kirshner et al, ApJ, 320, 602, (1987), showed an emission temperature of 15,000 K that was already declining rapidly. Ultraviolet observations later (Fransson et al, ApJ, 336, 429 (1989) showed narrow emission lines of N III, N IV, N V, and C III (all in the 1 ...
Cosmic Dawn A Hunting for the First Stars in the Universe
... of these secondary elements backwards in time, we can infer the existence of generations of stars that have long since disappeared, in much the same way that an archeologist peels back geological strata to map the fossil record of extinct species. What astronomers call the “pollution” of the univer ...
... of these secondary elements backwards in time, we can infer the existence of generations of stars that have long since disappeared, in much the same way that an archeologist peels back geological strata to map the fossil record of extinct species. What astronomers call the “pollution” of the univer ...
1 Sun Stars Planets. Problem Sheet I
... (d) By finding also how effective temperature Teff scales with mass for these stars, deduce a relation between log L and log Teff. 8. A main sequence star with the same radius as the Sun has a maximum energy output in visible light at a wavelength of 500 nm. If this star goes on to become a red gian ...
... (d) By finding also how effective temperature Teff scales with mass for these stars, deduce a relation between log L and log Teff. 8. A main sequence star with the same radius as the Sun has a maximum energy output in visible light at a wavelength of 500 nm. If this star goes on to become a red gian ...
Contents ISP 205 Section 2 Study Guide for Test 3 28 March 2007
... White dwarfs are earth-sized, dead stars. Degenerate electrons produce the pressure. Neutron stars are Lansing-sized stars made of degenerate neutrons Black holes are so compact that light cannot escape from them. Exploding stars, supernovae, spew elements into space. Planets form near other stars. ...
... White dwarfs are earth-sized, dead stars. Degenerate electrons produce the pressure. Neutron stars are Lansing-sized stars made of degenerate neutrons Black holes are so compact that light cannot escape from them. Exploding stars, supernovae, spew elements into space. Planets form near other stars. ...
Lecture
... • First stage: all stars start fusing hydrogen (H) to make helium (He) • This stage is considered to be the longest stage in a star’s lifetime ( 90% of its total lifespan) • Second stage: Fusing of helium (He) to make carbon (C) • The life of some stars (like our Sun) stops after this stage, but ot ...
... • First stage: all stars start fusing hydrogen (H) to make helium (He) • This stage is considered to be the longest stage in a star’s lifetime ( 90% of its total lifespan) • Second stage: Fusing of helium (He) to make carbon (C) • The life of some stars (like our Sun) stops after this stage, but ot ...
Question 1 The star Regulus, in the constellation Leo, appears
... . 2. elliptical galaxies with bright, starlike nuclei. ...
... . 2. elliptical galaxies with bright, starlike nuclei. ...
Chapter 13 Neutron Stars and Black Holes
... The mass of a neutron star cannot exceed about 3 solar masses. If a core remnant is more massive than that, nothing will stop its collapse, and it will become smaller and smaller and denser and denser. Eventually the gravitational force is so intense that even light cannot escape. The remnant has be ...
... The mass of a neutron star cannot exceed about 3 solar masses. If a core remnant is more massive than that, nothing will stop its collapse, and it will become smaller and smaller and denser and denser. Eventually the gravitational force is so intense that even light cannot escape. The remnant has be ...
N5128PNSydney
... some higher values near centre (Field 42). Assuming most PN have similar stellar temperature and most of O in O++ => O/H abundance [Ne III]/[O III] very constant as found in other PN studies (MW, MC’s). Ne/O ratio ‘fixed’ by early high mass star evolution and marginal evidence for O enrichment by PN ...
... some higher values near centre (Field 42). Assuming most PN have similar stellar temperature and most of O in O++ => O/H abundance [Ne III]/[O III] very constant as found in other PN studies (MW, MC’s). Ne/O ratio ‘fixed’ by early high mass star evolution and marginal evidence for O enrichment by PN ...
Stellar Astrophysics: Introduction Q. Daniel Wang Astronomy Department University of Massachusetts
... where M is any constant. We then obtain, for example, M αr −1 ...
... where M is any constant. We then obtain, for example, M αr −1 ...