Radiation-driven Feedback to the ISM around AGNs
... hand, diffuse and relatively stable outflows with ρ ∼ 10−2 M pc−3 or less are formed in the less luminous model with LA G N /LE dd = 0.01. We found that when biconical radiation-driven outflows are formed, “back-flows” toward the disk plane also appear outside the outflows. These accretion flows interact ...
... hand, diffuse and relatively stable outflows with ρ ∼ 10−2 M pc−3 or less are formed in the less luminous model with LA G N /LE dd = 0.01. We found that when biconical radiation-driven outflows are formed, “back-flows” toward the disk plane also appear outside the outflows. These accretion flows interact ...
The Westerbork Hydrogen Accretion in LOcal GAlaxieS \(HALOGAS
... of the four targets which have been observed in the pilot survey described in this paper are indicated with a bold font. The galaxy parameters listed in Table 1 are taken from Tully (1988), except for vrot , which is from HyperLEDA (Paturel et al. 2003), the adopted distance dbest , and the SFR, bot ...
... of the four targets which have been observed in the pilot survey described in this paper are indicated with a bold font. The galaxy parameters listed in Table 1 are taken from Tully (1988), except for vrot , which is from HyperLEDA (Paturel et al. 2003), the adopted distance dbest , and the SFR, bot ...
Modelling galaxy spectra in presence of interstellar dust – II. From
... three main components: (i) the diffuse interstellar medium (ISM) composed of gas and dust, (ii) the large complexes of molecular clouds (MCs) in which new stars are formed and (iii) the stars of any age and chemical composition. The galaxy models stand on a robust model of chemical evolution that as ...
... three main components: (i) the diffuse interstellar medium (ISM) composed of gas and dust, (ii) the large complexes of molecular clouds (MCs) in which new stars are formed and (iii) the stars of any age and chemical composition. The galaxy models stand on a robust model of chemical evolution that as ...
Mysterious transient objects - NCRA
... •Life time of stars ~ millions to billions of years Some sources appear in the sky for few seconds to few months to few years…. Transient objects ...
... •Life time of stars ~ millions to billions of years Some sources appear in the sky for few seconds to few months to few years…. Transient objects ...
PRESENT-DAY CLUSTER FORMATION
... example, that the main effect of the earlier episodes of star formation is actually to disperse the residual gas, and that only some fraction of this gas, perhaps that which was already in clumps, is compressed into denser clumps which then form compact clusters of stars. The primary triggering effe ...
... example, that the main effect of the earlier episodes of star formation is actually to disperse the residual gas, and that only some fraction of this gas, perhaps that which was already in clumps, is compressed into denser clumps which then form compact clusters of stars. The primary triggering effe ...
aaswinter06
... monitoring the masers with the Very Large Array. Since September, 2005, we have observed the masers for 5 epochs with the VLA, separated by approximately 1-month intervals. The most recent VLA spectra are shown in Figure 1. Figure 2 shows the time history of the peak maser fluxes. In addition, we ob ...
... monitoring the masers with the Very Large Array. Since September, 2005, we have observed the masers for 5 epochs with the VLA, separated by approximately 1-month intervals. The most recent VLA spectra are shown in Figure 1. Figure 2 shows the time history of the peak maser fluxes. In addition, we ob ...
A Tour of the Radio Universe
... the sharp Hubble images. Most of the pale, white objects sprinkled around the body of M82 that look like fuzzy stars are actually individual star clusters about 20 light-years across and contain up to a million stars. The rapid rate of star formation in this galaxy eventually will be self-limiting. ...
... the sharp Hubble images. Most of the pale, white objects sprinkled around the body of M82 that look like fuzzy stars are actually individual star clusters about 20 light-years across and contain up to a million stars. The rapid rate of star formation in this galaxy eventually will be self-limiting. ...
Part 2 - Aryabhat
... All stars shine but none do it like Sirius, the brightest star in the night sky. Aptly named, Sirius comes from the Greek word Seirius, meaning, "searing" or "scorching." Blazing at a visual magnitude of –1.42, it is twice as bright as any other star in our sky. Sirius resides in the constellation C ...
... All stars shine but none do it like Sirius, the brightest star in the night sky. Aptly named, Sirius comes from the Greek word Seirius, meaning, "searing" or "scorching." Blazing at a visual magnitude of –1.42, it is twice as bright as any other star in our sky. Sirius resides in the constellation C ...
- UCL Discovery
... where C∗ is a dimensionless SFR parameter and tg is the dynamical time. We set C∗ = 1, which is rather large, compared to C∗ ∼ 0.02 often used in these kind of simulations, including our previous work (Rahimi & Kawata 2012). However, note that the pressure of the gas particle becomes less than PJean ...
... where C∗ is a dimensionless SFR parameter and tg is the dynamical time. We set C∗ = 1, which is rather large, compared to C∗ ∼ 0.02 often used in these kind of simulations, including our previous work (Rahimi & Kawata 2012). However, note that the pressure of the gas particle becomes less than PJean ...
The evolution of dwarf galaxy satellites with different dark matter
... Group carried out in a fully cosmological context. We use the ErisDARK cosmological simulation of a MW-sized galaxy to identify some of the most massive subhalos (Mvir > 108 M ) that fall into the main host before z = 2. Subhalos are replaced before infall with high-resolution models of dwarf galax ...
... Group carried out in a fully cosmological context. We use the ErisDARK cosmological simulation of a MW-sized galaxy to identify some of the most massive subhalos (Mvir > 108 M ) that fall into the main host before z = 2. Subhalos are replaced before infall with high-resolution models of dwarf galax ...
Strongly Interacting Supernovae - The National Centre for Radio
... NH=1.3x1021 cm-2 (Galactic 4.5x1020 cm-2) Detection of 6.9 keV Fe XXVI line (EW=1.4 keV). Possible detection of 8.1 keV Ni XXVIII line 5Msun Mekal fits the data well and reproduces Fe line. NEI model also fits data well but reproduces very low density ~7E-3 cm-3. ...
... NH=1.3x1021 cm-2 (Galactic 4.5x1020 cm-2) Detection of 6.9 keV Fe XXVI line (EW=1.4 keV). Possible detection of 8.1 keV Ni XXVIII line 5Msun Mekal fits the data well and reproduces Fe line. NEI model also fits data well but reproduces very low density ~7E-3 cm-3. ...
Ellipticity, Its Origin and Progression in Comoving Galaxies
... packed array of rhombic dodecahedra (as well as trapezoidal-rhombic dodecahedra), which means that they fit together so as to divide up a volume of space without leaving gaps between adjacent cells. Furthermore, from a gravitational point of view, the universe is a packed array of tetrahedral and oc ...
... packed array of rhombic dodecahedra (as well as trapezoidal-rhombic dodecahedra), which means that they fit together so as to divide up a volume of space without leaving gaps between adjacent cells. Furthermore, from a gravitational point of view, the universe is a packed array of tetrahedral and oc ...
The cosmic distance scale
... individual Cepheids can be resolved as far away as the Virgo cluster of galaxies. Cepheids have periods from a few to about 70 days and this depends on their absolute magnitudes. In Table 1 HST observations of six Cepheids are listed. They were observed at 12 epochs (times) in order to find their pe ...
... individual Cepheids can be resolved as far away as the Virgo cluster of galaxies. Cepheids have periods from a few to about 70 days and this depends on their absolute magnitudes. In Table 1 HST observations of six Cepheids are listed. They were observed at 12 epochs (times) in order to find their pe ...
The Primordial Abundance of $^ 6$ Li and $^ 9$ be
... of α-element enhancement may be accounted for by modifying the overall Z of the star, as outlined by Salaris, Chieffi & Straniero 1993) and so is the most appropriate isochrone to compare to the observation. If HD 84937 is a main sequence star, then the models predict that the protostellar 6 Li has ...
... of α-element enhancement may be accounted for by modifying the overall Z of the star, as outlined by Salaris, Chieffi & Straniero 1993) and so is the most appropriate isochrone to compare to the observation. If HD 84937 is a main sequence star, then the models predict that the protostellar 6 Li has ...
Astronomy 112: The Physics of Stars Class 11 Notes: Stellar
... contrast, instability occurs when any small deviation from an equilibrium solution tends to drive the system further and further away from it. The classic example of an unstable system is a pencil standing on its point. If one could get the pencil to balance completely perfectly, it would be in equi ...
... contrast, instability occurs when any small deviation from an equilibrium solution tends to drive the system further and further away from it. The classic example of an unstable system is a pencil standing on its point. If one could get the pencil to balance completely perfectly, it would be in equi ...
A Search for New Solar-Type Post-T Tauri Stars in
... near- and far-ultraviolet universe. One area of astronomical research that is not well-served by the AIS, due to avoidance of the galactic plane, is young stars. According to Fischer (1998; PhD Thesis, UCSC) only 1% (2/189) of a volume-limited (d < 25 pc) sample of K stars have lithium abundances an ...
... near- and far-ultraviolet universe. One area of astronomical research that is not well-served by the AIS, due to avoidance of the galactic plane, is young stars. According to Fischer (1998; PhD Thesis, UCSC) only 1% (2/189) of a volume-limited (d < 25 pc) sample of K stars have lithium abundances an ...
I Introduction to the Interstellar Medium
... stars came from photographic spectroscopy of spectroscopic binary stars early in the 20th century. It was noticed that in addition to the relatively broad absorption lines associated with the atmospheres of the stars, there were very narrow lines that appeared stationary with respect to the cyclical ...
... stars came from photographic spectroscopy of spectroscopic binary stars early in the 20th century. It was noticed that in addition to the relatively broad absorption lines associated with the atmospheres of the stars, there were very narrow lines that appeared stationary with respect to the cyclical ...
Chemical composition of halo and disk stars with
... distribution in [Fe/H] for the two groups. Obviously, one cannot be sure that each individual star has been classified correctly as halo or disk, but the probability of correct classification seems high. The mean velocity of Galactic thick-disk stars is hVrot i ' 200 km s−1 and the dispersion is of ...
... distribution in [Fe/H] for the two groups. Obviously, one cannot be sure that each individual star has been classified correctly as halo or disk, but the probability of correct classification seems high. The mean velocity of Galactic thick-disk stars is hVrot i ' 200 km s−1 and the dispersion is of ...
CHP 11
... e. Giant molecular clouds Opacity is a. the balance between the pressure and force of gravity inside a star. b. the force that binds protons and neutrons together to form a nucleus. c. the force that binds an electron to the nucleus in an atom. d. a measure of the ease with which photons can pass th ...
... e. Giant molecular clouds Opacity is a. the balance between the pressure and force of gravity inside a star. b. the force that binds protons and neutrons together to form a nucleus. c. the force that binds an electron to the nucleus in an atom. d. a measure of the ease with which photons can pass th ...
the Local Group - Simon P Driver
... galaxies, e.g. send density waves through the gas – this leads to new bursts of star formation, perhaps as seen in the LMC irregular spiral • strong interactions can destroy galaxies as discrete entitities – some originally in the Local Group are now gone, all we see now are ‘tidal streams’ Galax ...
... galaxies, e.g. send density waves through the gas – this leads to new bursts of star formation, perhaps as seen in the LMC irregular spiral • strong interactions can destroy galaxies as discrete entitities – some originally in the Local Group are now gone, all we see now are ‘tidal streams’ Galax ...
CO emissions from optically selected galaxies at z ∼0.1–0.2: Tight
... galactic disks have evolved in z < 1 and both bulges and disk had been formed by z > 1 (e.g., van Dokkum et al. 2013). These indicate that the redshift range of z < 1 is the growing period for disk galaxies in terms of stellar mass. In addition, local disk galaxies have evolved their galactic disks ...
... galactic disks have evolved in z < 1 and both bulges and disk had been formed by z > 1 (e.g., van Dokkum et al. 2013). These indicate that the redshift range of z < 1 is the growing period for disk galaxies in terms of stellar mass. In addition, local disk galaxies have evolved their galactic disks ...
Massive Black Hole Growth and Formation
... where m p is the mass of the proton, σT is the Thomson cross-section, and ε 0.1 is the efÞciency at which accreting gas rest mass energy is converted in radiation expressed in units of 10%, the standard value for an accreting Schwarzchild black hole. (In terms of this efÞciency, the accretion lumin ...
... where m p is the mass of the proton, σT is the Thomson cross-section, and ε 0.1 is the efÞciency at which accreting gas rest mass energy is converted in radiation expressed in units of 10%, the standard value for an accreting Schwarzchild black hole. (In terms of this efÞciency, the accretion lumin ...
A new fitting-function to describe the time evolution of a galaxy`s
... also use a power-law relation between scale mass and scale radius to describe the growth of dark matter halos in cosmological simulations, except that we have found a general condition under which a system following a given density profile will grow inside out. Tasitsiomi et al. (2004) found that so ...
... also use a power-law relation between scale mass and scale radius to describe the growth of dark matter halos in cosmological simulations, except that we have found a general condition under which a system following a given density profile will grow inside out. Tasitsiomi et al. (2004) found that so ...