Cygnus X-1 poster (Massive Star Workshop)
... Background and Purpose Cygnus X-1 is a luminous X-ray binary, hosting a 14.81 ± 0.98 M⊙ black hole (BH) and a 19.16 ± 1.90 M⊙ O supergiant star in a Keplerian orbit of 5.6 days (Orosz 2011). This system is a persistent X-ray source that emits in two states: low-hard or high-soft state. Although the ...
... Background and Purpose Cygnus X-1 is a luminous X-ray binary, hosting a 14.81 ± 0.98 M⊙ black hole (BH) and a 19.16 ± 1.90 M⊙ O supergiant star in a Keplerian orbit of 5.6 days (Orosz 2011). This system is a persistent X-ray source that emits in two states: low-hard or high-soft state. Although the ...
The University of Sydney Page
... Massive stars can reach temperatures in their core high enough to begin fusing carbon, producing neon and oxygen. When the carbon is exhausted in the core, it contracts and carbon ignites in a shell. This pattern of core ignition and shell ignition continues with fuel after fuel, until the star deve ...
... Massive stars can reach temperatures in their core high enough to begin fusing carbon, producing neon and oxygen. When the carbon is exhausted in the core, it contracts and carbon ignites in a shell. This pattern of core ignition and shell ignition continues with fuel after fuel, until the star deve ...
–1– 1. Introduction for AY 219 The periodic table of the elements
... radiation is always non-thermal. For our purposes, the most common source of γ-rays is from decays, particularly those of common elements made in massive stars, which we can expect to eject lots of energy into the ISM, and so expect extended emission in the Galactic plane with higher flux from known ...
... radiation is always non-thermal. For our purposes, the most common source of γ-rays is from decays, particularly those of common elements made in massive stars, which we can expect to eject lots of energy into the ISM, and so expect extended emission in the Galactic plane with higher flux from known ...
Adiabatic evolution of mass-losing stars
... The previous works generally assumed comparable masses of the two objects in the binary system and an unchanging distance between them throughout the process. In this paper, we will use real stellar models to study how stars respond under adiabatic mass-loss on a time-scale slower than the dynamical ...
... The previous works generally assumed comparable masses of the two objects in the binary system and an unchanging distance between them throughout the process. In this paper, we will use real stellar models to study how stars respond under adiabatic mass-loss on a time-scale slower than the dynamical ...
Interstellar Astrophysics Summary notes: Part 5
... collapses, the sizes of the fragments decreases. ...
... collapses, the sizes of the fragments decreases. ...
doc
... certain point, the newly forming object becomes visible. At this stage the large luminous body is called a protostar. The other half of its gravitational energy remains within the protostar as heat. As contraction continues, the internal temperature of the protostar keeps rising, and when it reaches ...
... certain point, the newly forming object becomes visible. At this stage the large luminous body is called a protostar. The other half of its gravitational energy remains within the protostar as heat. As contraction continues, the internal temperature of the protostar keeps rising, and when it reaches ...
Test Ch. 27 Multiple Choice Identify the choice that best completes
... 25. In the last stage of stellar evolution following a supernova, stars too massive to form neutron stars may form a A. black dwarf. B. red supergiant. C. white dwarf. D. black hole. 26. In which stage of stellar evolution does combined hydrogen fusion and helium fusion cause a star’s outer shell to ...
... 25. In the last stage of stellar evolution following a supernova, stars too massive to form neutron stars may form a A. black dwarf. B. red supergiant. C. white dwarf. D. black hole. 26. In which stage of stellar evolution does combined hydrogen fusion and helium fusion cause a star’s outer shell to ...
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... • The brightest and bluest, OB stars explode within a few million years, and thus don’t go far from the spiral arm where they were born ...
... • The brightest and bluest, OB stars explode within a few million years, and thus don’t go far from the spiral arm where they were born ...
... have been made for 8 nebulae, and several others are in progress. The results are given in Table 3, and are compared to abundances in the sun, B stars, an interstellar cloud and the Orion nebula (references are given in Pottasch & Beintema 1999). The accuracy of the values is difficult to estimate. ...
Stellar evolution – Part III of III - Inside Mines
... • The Iron core is likely more massive than the Chandrasekhar limit (1.4 M☉). • Therefore the electron pressure cannot balance the gravitational collapse, which occurs extremely quickly. Within 1/10th of a second, the collapse causes temperature to soar to 5x109 K! • In the core, the trapped g-rays ...
... • The Iron core is likely more massive than the Chandrasekhar limit (1.4 M☉). • Therefore the electron pressure cannot balance the gravitational collapse, which occurs extremely quickly. Within 1/10th of a second, the collapse causes temperature to soar to 5x109 K! • In the core, the trapped g-rays ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... twice—once 1.9 billion years ago and again 0.9 billion years ago—and that it is now coming in for a third collision in just another 10 million years. Until recently, most investigators have been studying how the Milky Way’s tremendous gravitational field and tidal forces are ripping the Sagittarius ...
... twice—once 1.9 billion years ago and again 0.9 billion years ago—and that it is now coming in for a third collision in just another 10 million years. Until recently, most investigators have been studying how the Milky Way’s tremendous gravitational field and tidal forces are ripping the Sagittarius ...
Dark Stars: Dark Matter annihilation can power the first stars
... Mass 1Gev-10TeV (take 100GeV) Annihilation via the weak force Same annihilation that leads to correct WIMP abundance in today’s universe persists in the Universe today wherever there is an overabundance of WIMPs Same annihilation that gives potentially observable signal in FERMI, PAMELA, etc ...
... Mass 1Gev-10TeV (take 100GeV) Annihilation via the weak force Same annihilation that leads to correct WIMP abundance in today’s universe persists in the Universe today wherever there is an overabundance of WIMPs Same annihilation that gives potentially observable signal in FERMI, PAMELA, etc ...
Unit 1 - mmRyan
... Now we reduce the distance to our final destination by 90% every ten seconds. Each step much smaller than the one before. ...
... Now we reduce the distance to our final destination by 90% every ten seconds. Each step much smaller than the one before. ...
PDF sample - Northern Central Hospital
... the first time, the reality of the previously hidden atomic world was beginning to make itself manifest. It is difficult today to fully appreciate how recent is the notion that atoms are real physical entities, and not mere mathematical or philosophical constructs. Even in 1906, scientists did not ...
... the first time, the reality of the previously hidden atomic world was beginning to make itself manifest. It is difficult today to fully appreciate how recent is the notion that atoms are real physical entities, and not mere mathematical or philosophical constructs. Even in 1906, scientists did not ...
WASP-120b, WASP-122b and WASP-123b: Three newly discovered
... provided to the full precision used in our calculations but times are only accurate to a few seconds at best. ...
... provided to the full precision used in our calculations but times are only accurate to a few seconds at best. ...
Progenitors and Hydrodynamics of Type II and lb Supernovae
... Does the series of flashes progress smoothly to the center or are some flashes so violent as to lead to envelope ejection several years before the supernova explodes (as Woosley & Weaver found)? Is an iron core ever produced? A proper study again requires the careful treatment of the burning. This t ...
... Does the series of flashes progress smoothly to the center or are some flashes so violent as to lead to envelope ejection several years before the supernova explodes (as Woosley & Weaver found)? Is an iron core ever produced? A proper study again requires the careful treatment of the burning. This t ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.