The rebirth of Supernova 1987A a study of the ejecta-ring collision
... total number of SNe, is therefore a result of deeper surveys of space to very high redshifts. The studies of very distant SNe, especielly Type Ia, have had major impacts on cosmology. Such observations have relativly recently shown that the Universe is expanding at an accelerating rate, which has in ...
... total number of SNe, is therefore a result of deeper surveys of space to very high redshifts. The studies of very distant SNe, especielly Type Ia, have had major impacts on cosmology. Such observations have relativly recently shown that the Universe is expanding at an accelerating rate, which has in ...
REVIEW Numerical Star-Formation Studies— A Status Report
... In the past, progress has only been achievable by dividing the problem into smaller bits and pieces and by focusing on few feedback loops. Stars of all ages radiate and will thus heat up physical processes or single scales only. Today, however, algothe gas in their vicinity. By doing so they influenc ...
... In the past, progress has only been achievable by dividing the problem into smaller bits and pieces and by focusing on few feedback loops. Stars of all ages radiate and will thus heat up physical processes or single scales only. Today, however, algothe gas in their vicinity. By doing so they influenc ...
THE GREAT AGN DEBATE `AGN VS STARBURST
... 5. Radio-quiet quasars/ and QSO (Quasi Stellar Object) are more luminous versions of Seyfert Type 1 galaxy. They show strong optical continuum emission, Xray continuum emission, and broad and narrow optical emission lines. Some astronomers use the term QSO for this object reserving 'quasar' for radi ...
... 5. Radio-quiet quasars/ and QSO (Quasi Stellar Object) are more luminous versions of Seyfert Type 1 galaxy. They show strong optical continuum emission, Xray continuum emission, and broad and narrow optical emission lines. Some astronomers use the term QSO for this object reserving 'quasar' for radi ...
Tidal interaction of a rotating 1 vec {M_sun} star with a - UvA-DARE
... frequency region where the (retrograde) high radial order g-mode resonances become tidally inefficient due to their rotational confinement to the stellar equator and strong damping by radiative losses. For still lower retrograde forcing frequencies we find a large number of closely spaced weakly dam ...
... frequency region where the (retrograde) high radial order g-mode resonances become tidally inefficient due to their rotational confinement to the stellar equator and strong damping by radiative losses. For still lower retrograde forcing frequencies we find a large number of closely spaced weakly dam ...
Population synthesis for symbiotic stars with white dwarf accretors
... rithm for angular momentum loss during the commonenvelope stages of evolution; Winters and his collaborators (Winters et al. 2000, 2002, 2003) studied the hydrodynamical structure of the stellar wind around AGB stars with low mass-loss rate and low wind outflow velocity. New observational catalogue a ...
... rithm for angular momentum loss during the commonenvelope stages of evolution; Winters and his collaborators (Winters et al. 2000, 2002, 2003) studied the hydrodynamical structure of the stellar wind around AGB stars with low mass-loss rate and low wind outflow velocity. New observational catalogue a ...
The eccentricities of the barium stars
... (1998) have recently reported Ba ii stars with periods well outside this range. Fig. 1 shows the observed eccentricity±period (e, P) diagrams and eccentricity distributions of Ba ii stars from Jorissen et al. (1998) and a similar set of normal giants from Boffin, Cerf & Paulus (1993). The sample of ...
... (1998) have recently reported Ba ii stars with periods well outside this range. Fig. 1 shows the observed eccentricity±period (e, P) diagrams and eccentricity distributions of Ba ii stars from Jorissen et al. (1998) and a similar set of normal giants from Boffin, Cerf & Paulus (1993). The sample of ...
NIR interferometry of the Seyfert galaxy NGC 1068
... to fit the SED of Rieke & Low (1975) with a K-band flux of 0.3 Jy. Most authors introduced in their extended torus an additional dust component located within the ionization cone to reach the required K band flux. Torus models which can explain the observed infrared SED by emission solely from the t ...
... to fit the SED of Rieke & Low (1975) with a K-band flux of 0.3 Jy. Most authors introduced in their extended torus an additional dust component located within the ionization cone to reach the required K band flux. Torus models which can explain the observed infrared SED by emission solely from the t ...
Observations of Jets and Outflows from Young Stars
... into a jet, with a velocity several times the escape-speed from the launch region, which can range from 100 to over 500 km s−1 . Internal shocks form where faster ejecta overrun slower material. The very fastest shocks can sometimes be detected in X-rays. These primary flows often contain molecules ...
... into a jet, with a velocity several times the escape-speed from the launch region, which can range from 100 to over 500 km s−1 . Internal shocks form where faster ejecta overrun slower material. The very fastest shocks can sometimes be detected in X-rays. These primary flows often contain molecules ...
Zapartas_deMink_Izzard_AA_2017
... expected to be ‘late’, that is, they occur with delay times longer than approximately 50 Myr, which is the maximum delay time expected for single stars. We show that these late events originate from progenitors in binary systems with most of them being of intermediate mass. We discuss these late ccS ...
... expected to be ‘late’, that is, they occur with delay times longer than approximately 50 Myr, which is the maximum delay time expected for single stars. We show that these late events originate from progenitors in binary systems with most of them being of intermediate mass. We discuss these late ccS ...
Dust in Proto-Planetary Disks: Properties and Evolution
... the dust mass is to go to longer wavelengths, where an increasing fraction of the disk becomes optically thin. Interferometric observations at millimeter and centimeter wavelengths have provided the strongest evidence so far that most of the original solid mass in protoplanetary disks has grown to c ...
... the dust mass is to go to longer wavelengths, where an increasing fraction of the disk becomes optically thin. Interferometric observations at millimeter and centimeter wavelengths have provided the strongest evidence so far that most of the original solid mass in protoplanetary disks has grown to c ...
Numerical Star-Formation Studies-
... The formation of stars is a key process in astrophysics. Detailed knowledge of the physical mechanisms that govern stellar birth is a prerequisite for understanding the formation and evolution of our galactic home, the Milky Way. A theory of star formation is an essential part of any model for the o ...
... The formation of stars is a key process in astrophysics. Detailed knowledge of the physical mechanisms that govern stellar birth is a prerequisite for understanding the formation and evolution of our galactic home, the Milky Way. A theory of star formation is an essential part of any model for the o ...
Constellation Guide Book
... People like to look at the stars at night. They want to see the constellations. Many people use constellation guides to help them find the constellations. These guides also include information about each constellation. Your assignment is to make a guide to fall constellations. You have an informatio ...
... People like to look at the stars at night. They want to see the constellations. Many people use constellation guides to help them find the constellations. These guides also include information about each constellation. Your assignment is to make a guide to fall constellations. You have an informatio ...
Constraining the Envelope Structure of L1527 IRS
... envelopes alone predicted too little flux short ward of 10µm, necessitating the inclusion of bipolar outflow cavities into the standard model (Calvet et al. 1994). Thus far, a simple bipolar cavity structure carved out of a TSC envelope has sufficed for modeling images and spectral energy distributi ...
... envelopes alone predicted too little flux short ward of 10µm, necessitating the inclusion of bipolar outflow cavities into the standard model (Calvet et al. 1994). Thus far, a simple bipolar cavity structure carved out of a TSC envelope has sufficed for modeling images and spectral energy distributi ...
PPT
... away from neutron star - corresponds well with optical wisps delineating termination shock boundary Patrick Slane ...
... away from neutron star - corresponds well with optical wisps delineating termination shock boundary Patrick Slane ...
arXiv:astro-ph/9701131v1 18 Jan 1997
... quietly fade from prominence as helium white dwarfs. This general evolutionary scenario is detailed in Figure 1 (adapted from Laughlin et al., 1996), which charts the path in the Hertzsprung-Russell diagram followed by low mass stars of several different masses in the range 0.08M⊙ ≤ M∗ ≤ 0.25M⊙. Upo ...
... quietly fade from prominence as helium white dwarfs. This general evolutionary scenario is detailed in Figure 1 (adapted from Laughlin et al., 1996), which charts the path in the Hertzsprung-Russell diagram followed by low mass stars of several different masses in the range 0.08M⊙ ≤ M∗ ≤ 0.25M⊙. Upo ...
File
... The last and final star is called the Alpheratz. This connects all three stars of Pegasus. It is the most prominent in the sky towards the end of Summer and through Autumn for the northern latitudes. ...
... The last and final star is called the Alpheratz. This connects all three stars of Pegasus. It is the most prominent in the sky towards the end of Summer and through Autumn for the northern latitudes. ...
The Space Density of Spiral Galaxies as f(magnitude, size and
... observed trends between stellar ages & metallicities and galaxy surface brightness parameters ...
... observed trends between stellar ages & metallicities and galaxy surface brightness parameters ...
The Spitzer/GLIMPSE Surveys - UW-Madison Astronomy
... IRDCs are cold, dense, molecular or dust clouds seen at MIR wavelengths in silhouette against the MIR background emission. They are the cradle of star formation and the repository of molecular gas in the Galaxy. IRDCs represent the densest condensations in giant molecular clouds and are the most lik ...
... IRDCs are cold, dense, molecular or dust clouds seen at MIR wavelengths in silhouette against the MIR background emission. They are the cradle of star formation and the repository of molecular gas in the Galaxy. IRDCs represent the densest condensations in giant molecular clouds and are the most lik ...
A SIGNIFICANTLY LOW CO ABUNDANCE TOWARD THE TW Hya
... Previous studies have attributed measured low CO abundances to gas-phase depletion by adsorption onto grains (Aikawa et al. 1996; Dartois et al. 2003). Under normal conditions CO freezes-out at low temperatures present in the midplane, T 20 K, where HD does not strongly emit, and therefore the red ...
... Previous studies have attributed measured low CO abundances to gas-phase depletion by adsorption onto grains (Aikawa et al. 1996; Dartois et al. 2003). Under normal conditions CO freezes-out at low temperatures present in the midplane, T 20 K, where HD does not strongly emit, and therefore the red ...
Cygnus X-1
Cygnus X-1 (abbreviated Cyg X-1) is a well-known galactic X-ray source, thought to be a black hole, in the constellation Cygnus. It was discovered in 1964 during a rocket flight and is one of the strongest X-ray sources seen from Earth, producing a peak X-ray flux density of 6977229999999999999♠2.3×10−23 Wm−2 Hz−1 (7003230000000000000♠2.3×103 Jansky). Cygnus X-1 was the first X-ray source widely accepted to be a black hole and it remains among the most studied astronomical objects in its class. The compact object is now estimated to have a mass about 14.8 times the mass of the Sun and has been shown to be too small to be any known kind of normal star, or other likely object besides a black hole. If so, the radius of its event horizon is about 7004440000000000000♠44 km.Cygnus X-1 belongs to a high-mass X-ray binary system about 7019574266339685654♠6070 ly from the Sun that includes a blue supergiant variable star designated HDE 226868 which it orbits at about 0.2 AU, or 20% of the distance from the Earth to the Sun. A stellar wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions of degrees, generating the observed X-rays. A pair of jets, arranged perpendicular to the disk, are carrying part of the energy of the infalling material away into interstellar space.This system may belong to a stellar association called Cygnus OB3, which would mean that Cygnus X-1 is about five million years old and formed from a progenitor star that had more than 7001400000000000000♠40 solar masses. The majority of the star's mass was shed, most likely as a stellar wind. If this star had then exploded as a supernova, the resulting force would most likely have ejected the remnant from the system. Hence the star may have instead collapsed directly into a black hole.Cygnus X-1 was the subject of a friendly scientific wager between physicists Stephen Hawking and Kip Thorne in 1975, with Hawking betting that it was not a black hole. He conceded the bet in 1990 after observational data had strengthened the case that there was indeed a black hole in the system. This hypothesis has not been confirmed due to a lack of direct observation but has generally been accepted from indirect evidence.