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arXiv:1505.07406v1 [hep-ph] 27 May 2015
... interactions in asymmetric nuclear matter, the structure and stability of exotic nuclei, the reaction dynamics induced by rare isotopes, the nature and evolution of neutron stars, and the mechanism of supernova explosion [1–7]. The symmetry energy also plays an important role in some interesting iss ...
... interactions in asymmetric nuclear matter, the structure and stability of exotic nuclei, the reaction dynamics induced by rare isotopes, the nature and evolution of neutron stars, and the mechanism of supernova explosion [1–7]. The symmetry energy also plays an important role in some interesting iss ...
The Life Cycles of Stars
... Black Holes- Black holes are another resulting body created after a supernova, usually having to be greater than at least 3.0 solar masses. When a star collapses at such a size, the stellar object becomes incredibly small and dense, resulting in a gravitational pull so powerful that radiation (heat) ...
... Black Holes- Black holes are another resulting body created after a supernova, usually having to be greater than at least 3.0 solar masses. When a star collapses at such a size, the stellar object becomes incredibly small and dense, resulting in a gravitational pull so powerful that radiation (heat) ...
Article PDF - IOPscience
... high inferred accretion rate onto the NS requires that the donor is in Roche-lobe overflow (RLO), as wind-fed X-ray binaries with NS accretors are expected to have X-ray luminosities orders of magnitude below the ULX range (Linden et al. 2010), (2) the donor star must be hydrogen rich, as a helium st ...
... high inferred accretion rate onto the NS requires that the donor is in Roche-lobe overflow (RLO), as wind-fed X-ray binaries with NS accretors are expected to have X-ray luminosities orders of magnitude below the ULX range (Linden et al. 2010), (2) the donor star must be hydrogen rich, as a helium st ...
FIRST LIGHT IN THE UNIVERSE
... formation in the Universe • We have a good understanding of the evolution of the co-moving density of SF since z~3 which accounts for the observed stellar mass density at z=0. Half the stars we see today were formed by z~2. • Galaxy populations identified by various means (sub-mm, LBGs, BzK, DRG..) ...
... formation in the Universe • We have a good understanding of the evolution of the co-moving density of SF since z~3 which accounts for the observed stellar mass density at z=0. Half the stars we see today were formed by z~2. • Galaxy populations identified by various means (sub-mm, LBGs, BzK, DRG..) ...
Chapter 25.2 - Planet Earth
... White Dwarfs White dwarfs are the remains of low-mass and medium-mass stars. They are extremely small stars with densities greater than any known material on Earth. Although some white dwarfs are no larger than Earth, the mass of such a dwarf can equal 1.4 times that of the sun. So, their densities ...
... White Dwarfs White dwarfs are the remains of low-mass and medium-mass stars. They are extremely small stars with densities greater than any known material on Earth. Although some white dwarfs are no larger than Earth, the mass of such a dwarf can equal 1.4 times that of the sun. So, their densities ...
Magnetars: properties, origin and evolution
... 2003; Woods et al. 2004; Dib et al. 2009). They involve fractional frequency changes ∆ ν/ν ∼ 10−7 − 10−4 , similar to those of the strongest glitches of radio pulsars (Dib et al. 2008), but the apparent paucity of magnetars glitches with smaller ∆ ν/ν is probably a selection effect. The relation bet ...
... 2003; Woods et al. 2004; Dib et al. 2009). They involve fractional frequency changes ∆ ν/ν ∼ 10−7 − 10−4 , similar to those of the strongest glitches of radio pulsars (Dib et al. 2008), but the apparent paucity of magnetars glitches with smaller ∆ ν/ν is probably a selection effect. The relation bet ...
Fundamentals of Radio Astronomy - Radio Observations of Active
... • Stars: Very low mass and brown dwarfs - some M+L type dwarfs, brown dwarfs show quiescent and flaring nonthermal emission (Berger et al. 2001-7; Hallinan et al. (2006,2008) <-- magnetic activity at the poles: electrons interact with dwarfʼs magnetic field to produce radio waves that then are ampl ...
... • Stars: Very low mass and brown dwarfs - some M+L type dwarfs, brown dwarfs show quiescent and flaring nonthermal emission (Berger et al. 2001-7; Hallinan et al. (2006,2008) <-- magnetic activity at the poles: electrons interact with dwarfʼs magnetic field to produce radio waves that then are ampl ...
X-ray and Gamma-ray Studies of the Millisecond Pulsar and
... indicates negligible probabilities of 4 × 10−94 (20.5σ ) and 2 × 10−14 (7.6σ ) that the observed flux variability arises from a constant flux distribution for XMM-Newton and Chandra, respectively. A more robust estimate is obtained from the Kuiper test (Paltani 2004), which considers the unbinned li ...
... indicates negligible probabilities of 4 × 10−94 (20.5σ ) and 2 × 10−14 (7.6σ ) that the observed flux variability arises from a constant flux distribution for XMM-Newton and Chandra, respectively. A more robust estimate is obtained from the Kuiper test (Paltani 2004), which considers the unbinned li ...
Presentazione di PowerPoint
... minimal), with a component due to the combined gravitational potential of stars, dust, gas, dark matter, and anything else contributing mass to within that region. Beyond the sphere of influence, the gravitational dominance of the SMBH quickly vanishes. ...
... minimal), with a component due to the combined gravitational potential of stars, dust, gas, dark matter, and anything else contributing mass to within that region. Beyond the sphere of influence, the gravitational dominance of the SMBH quickly vanishes. ...
1. Seyfert Galaxies
... spectra of the nuclei of “spiral nebulae” and noted that NGC 1068 had strong emission lines Slipher obtained a higher quality spectrum at Lowell in 1917, noted the lines were similar to planetary nebulae In 1926, Hubble noted 3 galaxies with strong emission lines: NGC 1068, NGC 4051, NGC 4151 In 194 ...
... spectra of the nuclei of “spiral nebulae” and noted that NGC 1068 had strong emission lines Slipher obtained a higher quality spectrum at Lowell in 1917, noted the lines were similar to planetary nebulae In 1926, Hubble noted 3 galaxies with strong emission lines: NGC 1068, NGC 4051, NGC 4151 In 194 ...
Astro 3303 - Cornell Astronomy
... • The sky is dark at night. • Hubble’s Law & the expansion of the Universe (Edwin Hubble: 1927) • If the universe is finite in space and time and is expanding, it must have been smaller in the past. • The Cosmic Microwave Background (CMB) Radiation (Arno Penzias and Robert Wilson: 1965) • Thermal sp ...
... • The sky is dark at night. • Hubble’s Law & the expansion of the Universe (Edwin Hubble: 1927) • If the universe is finite in space and time and is expanding, it must have been smaller in the past. • The Cosmic Microwave Background (CMB) Radiation (Arno Penzias and Robert Wilson: 1965) • Thermal sp ...
Slide 1
... Pulsars (ie objects which emit radio pulses with very short periods) are isolated, highly magnetic neutron stars which radiate energy produced in the slowing down of their rapid spinning motion. Their rotational period is generally less than 1 second and the period is increasing with time. Neutron s ...
... Pulsars (ie objects which emit radio pulses with very short periods) are isolated, highly magnetic neutron stars which radiate energy produced in the slowing down of their rapid spinning motion. Their rotational period is generally less than 1 second and the period is increasing with time. Neutron s ...
G060324-00 - DCC
... Rate from Population Synthesis The good news: Population synthesis predicts: ...
... Rate from Population Synthesis The good news: Population synthesis predicts: ...
The Death of Massive Stars
... • Upper limit of Star’s Mass: Astronomers calculate that a star with a mass greater than 100 solar masses will emit radiation so intense that it will prevent more material from falling into the star, thereby limiting the star’s size. • Lower limit of Star’s Mass: Protostars with masses of less than ...
... • Upper limit of Star’s Mass: Astronomers calculate that a star with a mass greater than 100 solar masses will emit radiation so intense that it will prevent more material from falling into the star, thereby limiting the star’s size. • Lower limit of Star’s Mass: Protostars with masses of less than ...
Galaxies - Stockton University
... feeble emitters of radio waves in general. Some galaxies are much more powerful at radio wavelengths than normal. They can exceed the Milky Way by 103 to 107 times. These are radio galaxies. When resolved many have a double-lobe appearance in which two large lobes some hundred of kiloparsecs apart e ...
... feeble emitters of radio waves in general. Some galaxies are much more powerful at radio wavelengths than normal. They can exceed the Milky Way by 103 to 107 times. These are radio galaxies. When resolved many have a double-lobe appearance in which two large lobes some hundred of kiloparsecs apart e ...
a thermonuclear flame has almost completed TEN SECONDS AFTER IGNITION,
... problem is that deflagration should eject a large fraction of the white dwarf essentially unchanged, whereas observations suggest that at most a small part of the star remains unaltered. So the explosion cannot be a pure deflagration; some detonation must be involved. Theorists have yet to explain why ...
... problem is that deflagration should eject a large fraction of the white dwarf essentially unchanged, whereas observations suggest that at most a small part of the star remains unaltered. So the explosion cannot be a pure deflagration; some detonation must be involved. Theorists have yet to explain why ...
Neutron stars: compact objects with relativistic gravity
... some of the youngest ones, have been associated with supernova remnants. Not all pulsars have an associated supernova remnant because the life span of pulsars is two orders of magnitude larger than that of supernova remnants [78]. Neutron stars were also discovered as X-ray pulsars [79]. These are g ...
... some of the youngest ones, have been associated with supernova remnants. Not all pulsars have an associated supernova remnant because the life span of pulsars is two orders of magnitude larger than that of supernova remnants [78]. Neutron stars were also discovered as X-ray pulsars [79]. These are g ...
Coronal Mass Ejections and Angular Momentum Loss in Young Stars
... happens when stability is lost: at many stellar radii, is the specific angular momentum shed significant enough to slow stellar rotation? In order to estimate the effects of eruptive prominences and stellar CMEs on the rotation of young stars, we must procure two ingredients: the mass lost via these ...
... happens when stability is lost: at many stellar radii, is the specific angular momentum shed significant enough to slow stellar rotation? In order to estimate the effects of eruptive prominences and stellar CMEs on the rotation of young stars, we must procure two ingredients: the mass lost via these ...
Document
... What is this nothing which the gas and stars are rapidly orbiting? Only real possibility is a Black Hole! Must have a mass of 2.7£106M¯. Not a black hole from a single stellar collapse, but must be built up over time. We shall meet these again when we come to look at quasars, but we have to ask “Jus ...
... What is this nothing which the gas and stars are rapidly orbiting? Only real possibility is a Black Hole! Must have a mass of 2.7£106M¯. Not a black hole from a single stellar collapse, but must be built up over time. We shall meet these again when we come to look at quasars, but we have to ask “Jus ...
L95 IRON-RICH EJECTA IN THE SUPERNOVA
... A distinguishing characteristic of Type Ia supernovae (SNe Ia) is the large amount of iron that they are thought to produce mainly through the decay of radioactive 56Ni. The nuclear decay of this material powers the SN light curve, thereby providing a constraint on the quantity of material ejected i ...
... A distinguishing characteristic of Type Ia supernovae (SNe Ia) is the large amount of iron that they are thought to produce mainly through the decay of radioactive 56Ni. The nuclear decay of this material powers the SN light curve, thereby providing a constraint on the quantity of material ejected i ...
Astronomers discovered what they thought was the first black hole
... and his colleagues say the system was born between 8.7 and 11.4 million years ago with two massive stars orbiting each other. The more massive star – the one that is now the black hole – was born at least 110 times heavier than the Sun, making it one of the most luminous stars in the galaxy. Its par ...
... and his colleagues say the system was born between 8.7 and 11.4 million years ago with two massive stars orbiting each other. The more massive star – the one that is now the black hole – was born at least 110 times heavier than the Sun, making it one of the most luminous stars in the galaxy. Its par ...
Lecture 11 - University of Washington
... • Why there is an age spread of ∼ 3 Gyr among globular clusters (GCs)? We would expect < 1 Gyr spread (free-fall time). Some important questions that are left without robust answers: • Why GCs become more metal-poor with the distance from the center? • Detailed calculations of chemical enrichment pr ...
... • Why there is an age spread of ∼ 3 Gyr among globular clusters (GCs)? We would expect < 1 Gyr spread (free-fall time). Some important questions that are left without robust answers: • Why GCs become more metal-poor with the distance from the center? • Detailed calculations of chemical enrichment pr ...
Supermassive Black Holes and the Growth of Galaxies
... Since black holes by definition cannot emit light, an obvious question is how do we observe them? While we cannot see black holes directly, we can observe how their strong gravitational fields influence the matter and gas around them. At present observations have revealed two separate types of black ...
... Since black holes by definition cannot emit light, an obvious question is how do we observe them? While we cannot see black holes directly, we can observe how their strong gravitational fields influence the matter and gas around them. At present observations have revealed two separate types of black ...
Quasars: Back to the Infant Universe
... to our Galaxy (~ 60 million light years away in the Virgo Cluster) ! M87 has a huge radio jet, about 5000 light-years long ...
... to our Galaxy (~ 60 million light years away in the Virgo Cluster) ! M87 has a huge radio jet, about 5000 light-years long ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.