Astrophysical Sources of Gravitational Waves
... the angle between the two polarization states is π/4 rather than π/2.[1] ...
... the angle between the two polarization states is π/4 rather than π/2.[1] ...
Document
... do with galactic fountains? • When numerous supernovae occur relatively near each other and within a few million years of each other, the shock waves from the individual events may merge to form an enormous superbubble. In some places, superbubbles may blow through the galactic disk, creating a foun ...
... do with galactic fountains? • When numerous supernovae occur relatively near each other and within a few million years of each other, the shock waves from the individual events may merge to form an enormous superbubble. In some places, superbubbles may blow through the galactic disk, creating a foun ...
Diapositiva 1
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) ...
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) ...
Chapter 16 - Astronomy
... 2. Because the presence of dust and gas in the Galactic plane dims visible light from the nucleus, it wasn’t until the development of IR/radio and X-ray/gamma-ray astronomy that we could “look” at the Galactic nucleus. 3. The observed number density of stars increases as we get closer to the Galacti ...
... 2. Because the presence of dust and gas in the Galactic plane dims visible light from the nucleus, it wasn’t until the development of IR/radio and X-ray/gamma-ray astronomy that we could “look” at the Galactic nucleus. 3. The observed number density of stars increases as we get closer to the Galacti ...
Diapositiva 1
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) Italian contribution: Training data Galaxy simulation Cool star classification Not involv ...
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) Italian contribution: Training data Galaxy simulation Cool star classification Not involv ...
FREE Sample Here
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) The galaxy is about 100,000 light-years in diameter. D) One rotation of the galaxy takes about 200 million years. Answer: B 25) Which of the following correctl ...
Chapter 31
... – Sagittarius A*, the center of the galaxy, has about 2.6 million times the mass of the Sun but is smaller than our solar system. – Data gathered by the Chandra X-Ray Observatory reveal intense X-ray emissions as well. – Astronomers believe that Sagittarius A* is a supermassive black hole that proba ...
... – Sagittarius A*, the center of the galaxy, has about 2.6 million times the mass of the Sun but is smaller than our solar system. – Data gathered by the Chandra X-Ray Observatory reveal intense X-ray emissions as well. – Astronomers believe that Sagittarius A* is a supermassive black hole that proba ...
The Extragalactic Group of MPE and USM
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
AGN surveys to study galaxy evolution along cosmic times
... “The observed line intensities [....] in NGC1068 and 4151 closely resemble the line intensities of the planetary nebula NGC7027” and “The hydrogen lines in NGC4151 and 7469 are of unusual interest, being composed of relatively narrow cores (1100 km/sec wide) superposed on very wide wings (7500 km/se ...
... “The observed line intensities [....] in NGC1068 and 4151 closely resemble the line intensities of the planetary nebula NGC7027” and “The hydrogen lines in NGC4151 and 7469 are of unusual interest, being composed of relatively narrow cores (1100 km/sec wide) superposed on very wide wings (7500 km/se ...
Supernovae
... They are stars in the later stages of stellar evolution that suddenly contract and then explode, increasing their energy output by several orders of magnitude, which is from afar seen as a great increase in brightness of the progenitor star. After weeks or months these bright objects slowly decline ...
... They are stars in the later stages of stellar evolution that suddenly contract and then explode, increasing their energy output by several orders of magnitude, which is from afar seen as a great increase in brightness of the progenitor star. After weeks or months these bright objects slowly decline ...
Chapter 7: The Galaxy, structure and content File
... The term thick disc is usually given to a distribution of stars that is more extended in the vertical direction (perpendicular to the plane) than the main Galactic disc (the thin disc). The term is associated with stars, not gas. It consists of moderately metalpoor, older stars, with [Fe/H] close to ...
... The term thick disc is usually given to a distribution of stars that is more extended in the vertical direction (perpendicular to the plane) than the main Galactic disc (the thin disc). The term is associated with stars, not gas. It consists of moderately metalpoor, older stars, with [Fe/H] close to ...
poster208
... emission misses the 850μm peak in 5 sources, as expected in case of CO depletion (see Fig. 2 for an example). The median value for the integrated CO depletion factor is 3.2. III. Simple chemical models suggest that for the majority of the observed sources Dfrac and fD can be reproduced by gas temper ...
... emission misses the 850μm peak in 5 sources, as expected in case of CO depletion (see Fig. 2 for an example). The median value for the integrated CO depletion factor is 3.2. III. Simple chemical models suggest that for the majority of the observed sources Dfrac and fD can be reproduced by gas temper ...
Additional Cosmology Images
... young and were born from the same cloud of interstellar gas. The stars in an open cluster will only remain together for a limited time and gradually disperse into space, pulled away by the gravitational tugs of other passing clusters and clouds of gas. Most open clusters dissolve within a few hundre ...
... young and were born from the same cloud of interstellar gas. The stars in an open cluster will only remain together for a limited time and gradually disperse into space, pulled away by the gravitational tugs of other passing clusters and clouds of gas. Most open clusters dissolve within a few hundre ...
12 The Milky Way - Journigan-wiki
... from interstellar gas caught between the spiral arms of galaxies. The strong gravitational fields compress the gas creating stars that are gravitationally bound together. These clusters eventually break apart. Approximately 20,000 star clusters are believed to exist in the Milky Way. Our own Sun may ...
... from interstellar gas caught between the spiral arms of galaxies. The strong gravitational fields compress the gas creating stars that are gravitationally bound together. These clusters eventually break apart. Approximately 20,000 star clusters are believed to exist in the Milky Way. Our own Sun may ...
The Be/X-ray transient V0332153: evidence for a tilt between the
... accretion disc, was detected (Takeshima et al. 1994). V0332153 has not been detected by the BATSE experiment since the CGRO satellite started operations in 1991 April (Bildsten et al. 1997). It is not detected with any significance by the All-Sky Monitor (ASM) on board RXTE either, according to the ...
... accretion disc, was detected (Takeshima et al. 1994). V0332153 has not been detected by the BATSE experiment since the CGRO satellite started operations in 1991 April (Bildsten et al. 1997). It is not detected with any significance by the All-Sky Monitor (ASM) on board RXTE either, according to the ...
PHYS3380_111115_bw - The University of Texas at Dallas
... In the 1930’s supernovae were recognised as a separate class of objects to novae (meaning new stars). • So-called by Fritz Zwicky, after Edwin Hubble estimated distance to Andromeda galaxy (through Cepheids) • Hence the luminosity of the “nova” discovered in 1885 in Andromeda was determined • Supern ...
... In the 1930’s supernovae were recognised as a separate class of objects to novae (meaning new stars). • So-called by Fritz Zwicky, after Edwin Hubble estimated distance to Andromeda galaxy (through Cepheids) • Hence the luminosity of the “nova” discovered in 1885 in Andromeda was determined • Supern ...
Common Envelope Evolution Leading to Supernovae with Dense
... by a supernova can also be considered for the white dwarf case. A white dwarf spirals into the envelope of an evolved companion and continues to the core where strong accretion gives rise to a thermonuclear explosion. This scenario would be compatible with a double degenerate origin for Type Ia supe ...
... by a supernova can also be considered for the white dwarf case. A white dwarf spirals into the envelope of an evolved companion and continues to the core where strong accretion gives rise to a thermonuclear explosion. This scenario would be compatible with a double degenerate origin for Type Ia supe ...
Supernovae - University of Texas Astronomy Home Page
... find that such stars die in excess profusion. Stars with mass between about 8 and about 20 solar masses are born and die at the rate of about once per 100 years in our Galaxy. This is also the approximate rate at which we deduce Type II supernovae occur. Type II supernovae probably come from stars o ...
... find that such stars die in excess profusion. Stars with mass between about 8 and about 20 solar masses are born and die at the rate of about once per 100 years in our Galaxy. This is also the approximate rate at which we deduce Type II supernovae occur. Type II supernovae probably come from stars o ...
The Deaths of Very Massive Stars
... star to a level where it can frequently explode. If it does and the entire envelope has been lost, the explosion will be some sort of Type Ib or IC supernova. Because of the large mass, the light curve would be broad, and not as bright as most observed SN Ibc. The remnant would probably be a neutron ...
... star to a level where it can frequently explode. If it does and the entire envelope has been lost, the explosion will be some sort of Type Ib or IC supernova. Because of the large mass, the light curve would be broad, and not as bright as most observed SN Ibc. The remnant would probably be a neutron ...
The High Resolution Camera CXC Newsletter
... or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also ...
... or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also ...
Tod E. Strohmayer - UCLA Physics & Astronomy
... Extensive searches have been conducted for gravitationally redshifted absorption features in isolated neutron stars. – Most neutron stars (so far) show no discrete spectral structure. – Several isolated neutron stars (including;1E1207.4-5209, RX J0720.4-3125, RX J1605.3+3249, RX J1308.6+2127) show ...
... Extensive searches have been conducted for gravitationally redshifted absorption features in isolated neutron stars. – Most neutron stars (so far) show no discrete spectral structure. – Several isolated neutron stars (including;1E1207.4-5209, RX J0720.4-3125, RX J1605.3+3249, RX J1308.6+2127) show ...
Gamma-ray burst
Gamma-ray bursts (GRBs) are flashes of gamma rays associated with extremely energetic explosions that have been observed in distant galaxies. They are the brightest electromagnetic events known to occur in the universe. Bursts can last from ten milliseconds to several hours. The initial burst is usually followed by a longer-lived ""afterglow"" emitted at longer wavelengths (X-ray, ultraviolet, optical, infrared, microwave and radio).Most observed GRBs are believed to consist of a narrow beam of intense radiation released during a supernova or hypernova as a rapidly rotating, high-mass star collapses to form a neutron star, quark star, or black hole. A subclass of GRBs (the ""short"" bursts) appear to originate from a different process – this may be due to the merger of binary neutron stars. The cause of the precursor burst observed in some of these short events may be due to the development of a resonance between the crust and core of such stars as a result of the massive tidal forces experienced in the seconds leading up to their collision, causing the entire crust of the star to shatter.The sources of most GRBs are billions of light years away from Earth, implying that the explosions are both extremely energetic (a typical burst releases as much energy in a few seconds as the Sun will in its entire 10-billion-year lifetime) and extremely rare (a few per galaxy per million years). All observed GRBs have originated from outside the Milky Way galaxy, although a related class of phenomena, soft gamma repeater flares, are associated with magnetars within the Milky Way. It has been hypothesized that a gamma-ray burst in the Milky Way, pointing directly towards the Earth, could cause a mass extinction event.GRBs were first detected in 1967 by the Vela satellites, a series of satellites designed to detect covert nuclear weapons tests. Hundreds of theoretical models were proposed to explain these bursts in the years following their discovery, such as collisions between comets and neutron stars. Little information was available to verify these models until the 1997 detection of the first X-ray and optical afterglows and direct measurement of their redshifts using optical spectroscopy, and thus their distances and energy outputs. These discoveries, and subsequent studies of the galaxies and supernovae associated with the bursts, clarified the distance and luminosity of GRBs. These facts definitively placed them in distant galaxies and also connected long GRBs with the explosion of massive stars, the only possible source for the energy outputs observed.