2. The X-ray-Radio correlation for bulgeless galaxies
... The study of integrated light measurements in both the X-ray and Radio bands in galaxies allows for the identification of populations of new stars – and therefore, star formation processes – as well as markers for the presence of Active Galactic Nuclei. Correlations between the X-ray and Radio emiss ...
... The study of integrated light measurements in both the X-ray and Radio bands in galaxies allows for the identification of populations of new stars – and therefore, star formation processes – as well as markers for the presence of Active Galactic Nuclei. Correlations between the X-ray and Radio emiss ...
Extragalactic Background Light Encyclopedia of Astronomy & Astrophysics eaa.iop.org Rebecca A Bernstein
... at infrared wavelengths (λ 10 µm). Dust attenuation of short-wavelength light is very efficient and may prevent more than 30% of the star formation in the universe from being directly detected at wavelengths shorter than 1 µm. Non-stellar emission, such as the gravitational potential energy from a ...
... at infrared wavelengths (λ 10 µm). Dust attenuation of short-wavelength light is very efficient and may prevent more than 30% of the star formation in the universe from being directly detected at wavelengths shorter than 1 µm. Non-stellar emission, such as the gravitational potential energy from a ...
Radiation pressure from massive star clusters as a launching
... This cool gas can travel above the galactic disk in less than 2 Myr, well before any supernovae erupt in the driving cluster. Once above the disk, the cool outflowing gas is exposed to radiation, and supernovae induced hot gas outflows, from other clusters in the disk, which in combination drive it ...
... This cool gas can travel above the galactic disk in less than 2 Myr, well before any supernovae erupt in the driving cluster. Once above the disk, the cool outflowing gas is exposed to radiation, and supernovae induced hot gas outflows, from other clusters in the disk, which in combination drive it ...
(2004) - H. Peter
... higher “filling-factor” than Sun? not enough space on the surface and: also stellar X-rays are structured stellar corona are not only brighter, they have also high densities high temperatures ...
... higher “filling-factor” than Sun? not enough space on the surface and: also stellar X-rays are structured stellar corona are not only brighter, they have also high densities high temperatures ...
1987aj 93.1057n the astronomical journal volume 93, number 5 may
... much of the near-infrared flux of Arp 220, is clearly inadequate. An alternate possibility is that the unobserved source of the luminosity is a nonthermal source sufficiently obscured (e.g., with an^y ~ 100 mag) that it is not obvious at 2.2 jum and, possibly, not even at 3.7 jum. The possibility th ...
... much of the near-infrared flux of Arp 220, is clearly inadequate. An alternate possibility is that the unobserved source of the luminosity is a nonthermal source sufficiently obscured (e.g., with an^y ~ 100 mag) that it is not obvious at 2.2 jum and, possibly, not even at 3.7 jum. The possibility th ...
" Galaxy," Defined
... of galaxy that does not depend on a cold dark matter model of the universe: A galaxy is a gravitationally bound collection of stars whose properties cannot be explained by a combination of baryons and Newton’s laws of gravity. After exploring several possible observational diagnostics of this defini ...
... of galaxy that does not depend on a cold dark matter model of the universe: A galaxy is a gravitationally bound collection of stars whose properties cannot be explained by a combination of baryons and Newton’s laws of gravity. After exploring several possible observational diagnostics of this defini ...
FORMATION OF LATE-TYPE SPIRAL GALAXIES: GAS RETURN
... Supernovae account only for about 10% of this return fraction, which is dominated by low- and intermediate-mass stars. Half of ...
... Supernovae account only for about 10% of this return fraction, which is dominated by low- and intermediate-mass stars. Half of ...
Astrophysics in a Nutshell, Second Edition
... in each post-main-sequence evolution stage. Bottom: Theoretical stellar evolution tracks for stars of various initial main-sequence masses (with an assumed initial metal abundance of Z = 0.0004). Each track begins at the lower left end on the zero-age main sequence. After leaving the main sequence, ...
... in each post-main-sequence evolution stage. Bottom: Theoretical stellar evolution tracks for stars of various initial main-sequence masses (with an assumed initial metal abundance of Z = 0.0004). Each track begins at the lower left end on the zero-age main sequence. After leaving the main sequence, ...
Introduction_to_pulsar_astronomy
... neutron stars. He predicts a very slow and steady spin-down for these objects, based on the fact that they must be losing rotational energy due to their large EM emission. If the pulsations were due to vibration, then the intensity of the oscillation should decrease, and the vibration period (a char ...
... neutron stars. He predicts a very slow and steady spin-down for these objects, based on the fact that they must be losing rotational energy due to their large EM emission. If the pulsations were due to vibration, then the intensity of the oscillation should decrease, and the vibration period (a char ...
The significant contribution of minor mergers to the cosmic star
... Kewley et al. 2006). For galaxies classified as ‘star-forming’ (i.e. where the nuclear emission is dominated by star formation), SFRs are estimated by comparing galaxy spectra to a library of models based on Charlot & Longhetti (2001), with a dust treatment that follows the empirical model of Charlo ...
... Kewley et al. 2006). For galaxies classified as ‘star-forming’ (i.e. where the nuclear emission is dominated by star formation), SFRs are estimated by comparing galaxy spectra to a library of models based on Charlot & Longhetti (2001), with a dust treatment that follows the empirical model of Charlo ...
L53 He I 1.083 mm EMISSION AND ABSORPTION IN DG TAURI
... components are suggestive of their distinct origins, e.g., a fast jet and a slow disk wind (see Eislöffel et al. 2000). We present the results of long-slit spectroscopy and spectroastrometry for He i 1.083 mm and [Fe ii] 1.257 mm emission in DG Tauri. The former is one of the brightest among He i l ...
... components are suggestive of their distinct origins, e.g., a fast jet and a slow disk wind (see Eislöffel et al. 2000). We present the results of long-slit spectroscopy and spectroastrometry for He i 1.083 mm and [Fe ii] 1.257 mm emission in DG Tauri. The former is one of the brightest among He i l ...
4. Stars and resolved stellar populations
... wide-field 3D spectrograph would be uniquely powerful, to derive the details of chemical abundance and radial velocities for the majority of stars, especially in selected areas, with the Magellanic Clouds and the Bulge as obvious primary candidates (see e.g. Pasquini and Kissler 2002). Very dense st ...
... wide-field 3D spectrograph would be uniquely powerful, to derive the details of chemical abundance and radial velocities for the majority of stars, especially in selected areas, with the Magellanic Clouds and the Bulge as obvious primary candidates (see e.g. Pasquini and Kissler 2002). Very dense st ...
Cosmic Rays near Proxima Centauri b
... Sadovski 2017). Stellar cosmic rays (SCR) were considered in many papers (Tabataba-Vakili et al. 2016; Atri 2017; Struminsky & Sadovski 2017) as an important factor of space weather in a habitable zone of star. Since the details of SCR spectrum is unknown to model the effect of SCR one may use spect ...
... Sadovski 2017). Stellar cosmic rays (SCR) were considered in many papers (Tabataba-Vakili et al. 2016; Atri 2017; Struminsky & Sadovski 2017) as an important factor of space weather in a habitable zone of star. Since the details of SCR spectrum is unknown to model the effect of SCR one may use spect ...
Galaxy evolution - Pontifical Academy of Sciences
... rotating orthogonally to the other component. For example, in a stellar disk, the inner disk is rotating in the opposite direction of the outer disk, or the spheroidal component regarding the disk component. – Structural details in elliptical galaxies. For instance, elliptical galaxies with dust lan ...
... rotating orthogonally to the other component. For example, in a stellar disk, the inner disk is rotating in the opposite direction of the outer disk, or the spheroidal component regarding the disk component. – Structural details in elliptical galaxies. For instance, elliptical galaxies with dust lan ...
A FUSE Survey of Coronal Forbidden Lines in Late
... Because of our relatively poor knowledge of the rest wavelengths of these lines, the relatively weak signal of the coronal lines, and the moderate likelihood of coincidental blends with low-temperature lines, labeling spectral features located at wavelengths coincident with an expected coronal line ...
... Because of our relatively poor knowledge of the rest wavelengths of these lines, the relatively weak signal of the coronal lines, and the moderate likelihood of coincidental blends with low-temperature lines, labeling spectral features located at wavelengths coincident with an expected coronal line ...
The XXL Survey - I. Scientific motivations − XMM
... debated issue of cluster mass measurement. At intermediate redshift, XXL provides a unique census of the group population. The ∼250 clusters expected to be detected in the survey between 0.3 < z < 0.5 have masses around 5 × 1013 −1014 M . The XMM-LSS survey started systematically revealing this pop ...
... debated issue of cluster mass measurement. At intermediate redshift, XXL provides a unique census of the group population. The ∼250 clusters expected to be detected in the survey between 0.3 < z < 0.5 have masses around 5 × 1013 −1014 M . The XMM-LSS survey started systematically revealing this pop ...
Young Stellar Objects in the Orion B Cloud
... of the mass function, is remarkably similar to the Orion Trapezium KLF, which has been reported to have a fraction of substellar objects of ~ 22 % (Muench et al. 2002). We conclude that the star formation environment in Orion B is similarly productive in forming substellar objects as are more massiv ...
... of the mass function, is remarkably similar to the Orion Trapezium KLF, which has been reported to have a fraction of substellar objects of ~ 22 % (Muench et al. 2002). We conclude that the star formation environment in Orion B is similarly productive in forming substellar objects as are more massiv ...
Evidence for 1000 km/s Molecular Outflows in the Local ULIRG
... z = 0.043 − 0.11 (νrest = 110 − 120 GHz) shows broad wings around the CO line with ∆V (F W ZI) ≈ 2000 km s−1 . Its integrated line flux accounts for up to 25±5% of the total CO line luminosity. When interpreted as a massive molecular outflow wind, the associated mechanical energy can be explained by ...
... z = 0.043 − 0.11 (νrest = 110 − 120 GHz) shows broad wings around the CO line with ∆V (F W ZI) ≈ 2000 km s−1 . Its integrated line flux accounts for up to 25±5% of the total CO line luminosity. When interpreted as a massive molecular outflow wind, the associated mechanical energy can be explained by ...
RESEARCH STATEMENT Chromospheres and winds
... Manset, CFHT observing request 12BD001). The long history of observations of ε Aurigae paint a picture rich with features that may inform other similar studies. Energy propagation through the outer regions of the stellar atmosphere of the F0 star in the ε Aurigae system may be inferred from observat ...
... Manset, CFHT observing request 12BD001). The long history of observations of ε Aurigae paint a picture rich with features that may inform other similar studies. Energy propagation through the outer regions of the stellar atmosphere of the F0 star in the ε Aurigae system may be inferred from observat ...
Accreting millisecond X-ray pulsars: a search for pulsed radio
... collapse of a massive star (M ∼ supernova event, which occurs when a massive star runs out of nuclear fuel in its core at the end of its life. A typical neutron star has a mass between 1 M⊙ – 2.1 M⊙ , with a corresponding radius range of 8 – 15 km and then a resulting central density of 1014 −1015 g ...
... collapse of a massive star (M ∼ supernova event, which occurs when a massive star runs out of nuclear fuel in its core at the end of its life. A typical neutron star has a mass between 1 M⊙ – 2.1 M⊙ , with a corresponding radius range of 8 – 15 km and then a resulting central density of 1014 −1015 g ...
Detached WD/BD binaries as progenitors of CVs
... - CCD 2048 x 2048 pixels - Field of View 7.8 x 7.8 degrees (61 sq. degrees) - magnitude limit =15 V mag. - photometric accuracy of 1% down to 1 ...
... - CCD 2048 x 2048 pixels - Field of View 7.8 x 7.8 degrees (61 sq. degrees) - magnitude limit =15 V mag. - photometric accuracy of 1% down to 1 ...
talk
... FIGGS galaxies at highest resolution (~20-100 pc) Substantial fine scale structure visible at high resolution Scales of energy injection into ISM through stellar winds/supernovae ...
... FIGGS galaxies at highest resolution (~20-100 pc) Substantial fine scale structure visible at high resolution Scales of energy injection into ISM through stellar winds/supernovae ...
pps - TUM
... isotopes in the chain with neutron binding energy close to 3 MeV will tend to be the ones with maximum abundance. Keep in mind, that larger Nn will shift maxima to larger neutron number, and larger T will shift maximum to smaller neutron number along the chain. ...
... isotopes in the chain with neutron binding energy close to 3 MeV will tend to be the ones with maximum abundance. Keep in mind, that larger Nn will shift maxima to larger neutron number, and larger T will shift maximum to smaller neutron number along the chain. ...
Document
... 1. DC from E-fields ~ 103 Vm-1 during reconnection 2. MHD shocks - accelerate more particles more slowly - can explain the main phase 3. Highly turbulent environment may give rise to stochastic acceleration - ie fastmode Alfven-waves. ...
... 1. DC from E-fields ~ 103 Vm-1 during reconnection 2. MHD shocks - accelerate more particles more slowly - can explain the main phase 3. Highly turbulent environment may give rise to stochastic acceleration - ie fastmode Alfven-waves. ...
Galaxy Classification Much of modern extragalactic astronomy deals
... K supergiants. These objects are also the most condensed systems; i.e., they are highly concentrated. Irregular galaxies with no central mass condensation tend to have younger stars and a corresponding earlier spectral type. Thus, Morgan defined an “a-f-g-k” concentration index based on the spectral ...
... K supergiants. These objects are also the most condensed systems; i.e., they are highly concentrated. Irregular galaxies with no central mass condensation tend to have younger stars and a corresponding earlier spectral type. Thus, Morgan defined an “a-f-g-k” concentration index based on the spectral ...
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.