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Tersedia di Perpustakaan Universitas Pelita Bangsa
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Although the title points only to classical, shell SNR structures, the workshop also considered dynamical issues involving X-ray filled composite remnants and pulsar-driven shells, such as that in the Crab Nebula. Approximately 75 observers, theorists, and numerical simulators with wide-ranging interests attended the workshop. An even larger community helped through extensive on-line debates prior to the meeting to focus issues and galvanize discussion. In order to deflect thinking away from traditional patterns, the workshop was organized around chronological sessions for "very young," "young," "mature," and "old" remnants, with the implicit recognition that these labels are often difficult to apply. Special sessions were devoted to related issues in plerions and thermal X-ray composites. Controversy and debate were encouraged. Each session also addressed some underlying, general physical themes: How are supernova remnant (SNR) dynamics and structures modified by the character of the circumstellar medium (CSM) and the interstellar medium (ISM), and vice versa? How are magnetic fields generated in SNRs and how do magnetic fields influence SNRs? Where and how are cosmic rays (electrons and ions) produced in SNRs, and how does their presence influence or reveal SNR dynamics? How does SNR blast energy partition into various components over time, and what controls conversion between components? In lieu of a proceedings volume, we present here a synopsis of the workshop in the form of brief summaries of the workshop sessions. The sharpest impressions from the workshop were the crucial and under appreciated roles that environments have on SNR appearance and dynamics and the critical need for broad-based studies to understand these beautiful but enigmatic objects.
Special sessions were devoted to related issues in plerions and thermal X-ray composites. Controversy and debate were encouraged.
Please note that the content of this book primarily consists of articles available from Wikipedia or other free sources online. Pages: 59. Chapters: Vulture, Bart Allen, Damian Wayne, Neron, Magog, Superman, Osiris, Red Robin, Legion of Super-Heroes, Triumph, Supernova, Everyman, Cobalt Blue, Cyclone, Sobek, Norman McCay, Comet, Lady Styx, Agamemno, Firebird, Savitar, Offspring, Manfred Mota, Meloni Thawne, Dream Boy, Folded Man, Mercury. Excerpt: The Vulture is the name of six comic book supervillains in the Marvel Comics universe. The best known Vulture in the Marvel Universe is Adrian Toomes, an elderly enemy of Spider-Man created by Stan Lee and Steve Ditko in The Amazing Spider-Man #2 (May 1963). In Young Men #26, a scientist named Dr. Isidoro Scarlotti went by the name Vulture and was an enemy of the original Human Torch and Toro. Adrian Toomes was born in Staten Island, New York. He is a former electronics engineer who was once the business partner of a man named Gregory Bestman; Bestman handled the finances whilst Toomes handled the inventions. One day, after creating a flight harness, Toomes eagerly rushed into Bestman's office to share the happy news. However, Bestman was not there, and Toomes discovered that Bestman had secretly been embezzling funds and that Toomes had no legal recourse, meaning he lost his job. Enraged, Toomes wrecked the business, discovering that the harness also granted him superhuman strength. He then decided to turn to crime professionally as the Vulture. His wings are as sharp as swords and can be used as projectile weapons. They will replenish themselves so he can maintain flying abilities. The Vulture employs a special harness of his own design that allows him to fly; his flight is directed by a pair of wings worn on his arms. The harness also endows him with enhanced strength and (according to some sources) increases his lifespan. Although Toomes is advanced in age, he is a strong fighter and a remorseless killer. On one oc...
Please note that the content of this book primarily consists of articles available from Wikipedia or other free sources online.
One of the outstanding unsolved riddles of nuclear astrophysics is the origin of the so called ''p-process'' nuclei from A = 92 to 126. Both the lighter and heavier p-process nuclei are adequately produced in the neon and oxygen shells of ordinary Type II supernovae, but the origin of these intermediate isotopes, especially {sup 92,94}Mo and {sup 96,98}Ru, has long been mysterious. Here we explore the production of these nuclei in the neutrino-driven wind from a young neutron star. We consider such early times that the wind still contains a proton excess because the rates for [nu]{sub e} and positron captures on neutrons are faster than those for the inverse captures on protons. Following a suggestion by Froehlich et al. (2005), they also include the possibility that, in addition to the protons, [alpha]-particles, and heavy seed, a small flux of neutrons is maintained by the reaction p({bar {nu}}{sub e}, e)n. This flux of neutrons is critical in bridging the long waiting points along the path of the rp-process by (n, p) and (n, [gamma]) reactions. Using the unmodified ejecta histories from a recent two-dimensional supernova model by Janka, Buras, and Rampp (2003), they find synthesis of p-rich nuclei up to 1°2Pd. However, if the entropy of these ejecta is increased by a factor of two, the synthesis extends to 12°Te. Still larger increases in entropy, that might reflect the role of magnetic fields or vibrational energy input neglected in the hydrodynamical model, result in the production of numerous r-, s-, and p-process nuclei up to A H"170, even in winds that are proton-rich.
One of the outstanding unsolved riddles of nuclear astrophysics is the origin of the so called ''p-process'' nuclei from A = 92 to 126.
Recounts how the supernova was discovered and discusses the information it is providing scientists about the life cycle of stars
Recounts how the supernova was discovered and discusses the information it is providing scientists about the life cycle of stars
