The PAH emission spectra of Large Magellanic Cloud H II regions
... and even within 30 Doradus. The LMC spectra have been compared with ISO-SWS spectra from Galactic H ii regions and with the ISOCAM observation towards a quiescent molecular cloud in the SMC (Reach et al. 2000). A correlation is found between the I7.7 /I11.2 versus I6.2 /I11.2 and the I8.6 /I11.2 ver ...
... and even within 30 Doradus. The LMC spectra have been compared with ISO-SWS spectra from Galactic H ii regions and with the ISOCAM observation towards a quiescent molecular cloud in the SMC (Reach et al. 2000). A correlation is found between the I7.7 /I11.2 versus I6.2 /I11.2 and the I8.6 /I11.2 ver ...
Extragalactic Astronomical Masers I
... envelopes of evolved stars and starforming regions range from 0.001 Lʘ to 1 Lʘ, typically. H2O maser with a luminosity well above 1 Lʘ has never been found in our Galaxy. H 2O masers observed in nearby starforming or starburst galaxies with Liso values of 0.01―1 solar luminosity (Churchwell et al. ...
... envelopes of evolved stars and starforming regions range from 0.001 Lʘ to 1 Lʘ, typically. H2O maser with a luminosity well above 1 Lʘ has never been found in our Galaxy. H 2O masers observed in nearby starforming or starburst galaxies with Liso values of 0.01―1 solar luminosity (Churchwell et al. ...
Homi Bhabha
... also working at Cambridge had recorded several instances of multiple charged particles which had obvious non-ionising links between pairs of them. These events fitted beautifully the phenomenon of pair production or conversion of quanta into electron-positron pairs according to Dirac's theory. The c ...
... also working at Cambridge had recorded several instances of multiple charged particles which had obvious non-ionising links between pairs of them. These events fitted beautifully the phenomenon of pair production or conversion of quanta into electron-positron pairs according to Dirac's theory. The c ...
CEA
... GCN position notice (WXM) given 22 s after the beginning of the burst Raptor (LANL) observed 65 sec after burst Optical afterglow extremely faint after 2 hours GRB may have occurred on region with no surrouding gas or dust, so the shock wave had little material to smash into may support the binary ...
... GCN position notice (WXM) given 22 s after the beginning of the burst Raptor (LANL) observed 65 sec after burst Optical afterglow extremely faint after 2 hours GRB may have occurred on region with no surrouding gas or dust, so the shock wave had little material to smash into may support the binary ...
Sublimation temperature of circumstellar dust particles and its importance Hiroshi Kobayashi
... the particles lose their mass during sublimation, the ratio β of radiation pressure to gravity of the star acting on each particle ordinarily increases. As a result, their radial-drift rates decrease and the particles pile up at the outer edge of their sublimation zone (e.g., Mukai and Yamamoto, 197 ...
... the particles lose their mass during sublimation, the ratio β of radiation pressure to gravity of the star acting on each particle ordinarily increases. As a result, their radial-drift rates decrease and the particles pile up at the outer edge of their sublimation zone (e.g., Mukai and Yamamoto, 197 ...
SN 2011dh and the progenitors of Type IIb supernovae Mattias Ergon
... a billion Kelvin, oxygen burning will soon ignite, and in the six years that follows the temperature will continue to rise, the nuclear burning will proceed to silicon, and when the mass of the growing iron core reaches the Chandrasekhar limit at ∼12 UT the 30th of May 2011, the fate of the star is ...
... a billion Kelvin, oxygen burning will soon ignite, and in the six years that follows the temperature will continue to rise, the nuclear burning will proceed to silicon, and when the mass of the growing iron core reaches the Chandrasekhar limit at ∼12 UT the 30th of May 2011, the fate of the star is ...
STELLAR ABLATION OF PLANETARY ATMOSPHERES
... from the Sun, both electromagnetic and mechanical. The term ‘‘geospace’’ is used here in the sense suggested by the NSF Geospace Environment Modeling (GEM) Program, to encompass the coupled atmosphere, ionosphere, magnetosphere, and heliosphere. Over the past 40 years, the SunEarth system has been t ...
... from the Sun, both electromagnetic and mechanical. The term ‘‘geospace’’ is used here in the sense suggested by the NSF Geospace Environment Modeling (GEM) Program, to encompass the coupled atmosphere, ionosphere, magnetosphere, and heliosphere. Over the past 40 years, the SunEarth system has been t ...
The importance of radiative feedback for the stellar initial mass
... model) to provide the gas opacities (for further details, see Whitehouse & Bate 2006). The only change from Whitehouse & Bate (2006) is to do with the boundary condition. The clouds modelled here have free boundaries. To provide a boundary condition for the radiative transfer, all particles with den ...
... model) to provide the gas opacities (for further details, see Whitehouse & Bate 2006). The only change from Whitehouse & Bate (2006) is to do with the boundary condition. The clouds modelled here have free boundaries. To provide a boundary condition for the radiative transfer, all particles with den ...
The Limits of Our Solar System - Lunar and Planetary Institute
... of the interstellar He by about 4° (Lallement et al., 2005). This offset results from charge exchange of the H with the deflected H+ in front of the heliosphere. The direction of the offset tells us the direction of the plasma flow in the local interstellar cloud just outside the heliopause and thus ...
... of the interstellar He by about 4° (Lallement et al., 2005). This offset results from charge exchange of the H with the deflected H+ in front of the heliosphere. The direction of the offset tells us the direction of the plasma flow in the local interstellar cloud just outside the heliopause and thus ...
Probability of Solar Flares Turn Out to Form a Coronal Mass
... determined by the maximum phase of cycle 23 and the deep minimum of preliminary phase of cycle 24 [15]. Decade observations have also revealed that solar protons could sometimes be accelerated up to tens of GeV in some intense solar energetic process. The latest observations are extremely deficient ...
... determined by the maximum phase of cycle 23 and the deep minimum of preliminary phase of cycle 24 [15]. Decade observations have also revealed that solar protons could sometimes be accelerated up to tens of GeV in some intense solar energetic process. The latest observations are extremely deficient ...
Global Properties of Solar Flares
... fully equal to that of direct sun-light.” They occurred in small patches near a sunspot group. His description means that the flare was at least as bright as sunspots are dark, although the flare brightenings were much smaller in area and of course transient in nature, lasting only a few minutes. Hi ...
... fully equal to that of direct sun-light.” They occurred in small patches near a sunspot group. His description means that the flare was at least as bright as sunspots are dark, although the flare brightenings were much smaller in area and of course transient in nature, lasting only a few minutes. Hi ...
Solar Weather Event Modelling and Prediction
... indicating that the results obtained from ANN are in good agreement with the actual values. To date, such an approach seems to be the most promising and is widely used in prediction systems e.g. for sunspots and flares, as reported in Sects. 4.1.3 and 4.2.2. The chaotic nature of the Sun as a comple ...
... indicating that the results obtained from ANN are in good agreement with the actual values. To date, such an approach seems to be the most promising and is widely used in prediction systems e.g. for sunspots and flares, as reported in Sects. 4.1.3 and 4.2.2. The chaotic nature of the Sun as a comple ...
The energy spectrum of cosmic electrons measured with the MAGIC
... of up to 93 billion light years. However, not all cosmic rays are equally likely to reach the Earth from such distances. In particular the cosmic electrons on which this thesis will focus, reach Earth from much smaller distances. This is due to the strong energy losses they undergo in the magnetic f ...
... of up to 93 billion light years. However, not all cosmic rays are equally likely to reach the Earth from such distances. In particular the cosmic electrons on which this thesis will focus, reach Earth from much smaller distances. This is due to the strong energy losses they undergo in the magnetic f ...
Section IV High-Energy Astrophysics and Cosmology
... emission line at a half of height in the radiation spectrum, i.e. FWHM. The BLR radius RBLR is usually determined by the reverberation method, i.e. with time delay between continuum and emission line variations. Determination of the f value is strongly depending on accepted BLR model. Labita et al. ...
... emission line at a half of height in the radiation spectrum, i.e. FWHM. The BLR radius RBLR is usually determined by the reverberation method, i.e. with time delay between continuum and emission line variations. Determination of the f value is strongly depending on accepted BLR model. Labita et al. ...
SOLAR HARD X-RAY AND GAMMA-RAY OBSERVATIONS FROM
... 98 keV-1.5 MeV band for the 1990 February 11 event. The peaks marked 1, 3, and 4 are significant for an accumulation time of 250 ms, while peaks marked 2 and 5 are significant for accumulation times of 375 and 625 ms, respectively (Talon et al. 1993a). The systematic existence of subsecond time stru ...
... 98 keV-1.5 MeV band for the 1990 February 11 event. The peaks marked 1, 3, and 4 are significant for an accumulation time of 250 ms, while peaks marked 2 and 5 are significant for accumulation times of 375 and 625 ms, respectively (Talon et al. 1993a). The systematic existence of subsecond time stru ...
Miguel Pereira Santaella
... HF dissociated by intense UV radiation and reformed rapidly χ > 107 and high density nH2 > 107 cm-3 Possible close to the AGN ...
... HF dissociated by intense UV radiation and reformed rapidly χ > 107 and high density nH2 > 107 cm-3 Possible close to the AGN ...
Influence of extreme ultraviolet radiation on the Pv ionization fraction
... XUV radiation alone cannot bring theory and observations into agreement. We fit our predicted wind mass-loss rates using a suitable formula and we compare the results with the observational mass-loss rate diagnostics. We show that for supergiants and giants the theoretical predictions do not contrad ...
... XUV radiation alone cannot bring theory and observations into agreement. We fit our predicted wind mass-loss rates using a suitable formula and we compare the results with the observational mass-loss rate diagnostics. We show that for supergiants and giants the theoretical predictions do not contrad ...
Effects of Thomson-Scattering Geometry on White-Light
... inner heliosphere is not only determined by the local electron density, but also by Thomsonscattering theory. The Thomson-scattering geometry is defined by a sphere, on which the Sun and the observer are located on opposite ends of the diameter. The classical theory of Thomson scattering by Billings ...
... inner heliosphere is not only determined by the local electron density, but also by Thomsonscattering theory. The Thomson-scattering geometry is defined by a sphere, on which the Sun and the observer are located on opposite ends of the diameter. The classical theory of Thomson scattering by Billings ...
Quantum Theory of Neutrino Spin
... where µ0 = e/2m is the Bohr magneton, mν and m are the neutrino and electron masses, respectively. There are also models [2] in which much large values for magnetic moments of neutrinos are predicted. So far, the most stringent laboratory constraints on the electron, muon, and tau neutrino magnetic ...
... where µ0 = e/2m is the Bohr magneton, mν and m are the neutrino and electron masses, respectively. There are also models [2] in which much large values for magnetic moments of neutrinos are predicted. So far, the most stringent laboratory constraints on the electron, muon, and tau neutrino magnetic ...
radiation and matter interaction in strong magnetic field of accreting
... (huge temperatures, densities and magnetic fields) which by no means can be reached in terrestrial laboratories. The enormous strengths of NS magnetic fields (1011 − 1015 G) exceed values achieved by mankind by 10 orders of magnitude. As a result NSs permit us to study experimentally those areas of ...
... (huge temperatures, densities and magnetic fields) which by no means can be reached in terrestrial laboratories. The enormous strengths of NS magnetic fields (1011 − 1015 G) exceed values achieved by mankind by 10 orders of magnitude. As a result NSs permit us to study experimentally those areas of ...
Ionization in atmospheres of Brown Dwarfs and extrasolar planets IV
... are set to the solar values throughout this paper. We consider a model atmosphere of a brown dwarf, with a surface gravity of log g = 5 and an effective temperature of Teff = 1500 K, as well as model atmospheres for two example giant gas planets, both with log g = 3. The effective temperatures of fr ...
... are set to the solar values throughout this paper. We consider a model atmosphere of a brown dwarf, with a surface gravity of log g = 5 and an effective temperature of Teff = 1500 K, as well as model atmospheres for two example giant gas planets, both with log g = 3. The effective temperatures of fr ...
Health threat from cosmic rays
The health threat from cosmic rays is the danger posed by galactic cosmic rays and solar energetic particles to astronauts on interplanetary missions. Galactic cosmic rays (GCRs) consist of high energy protons (85%), helium (14%) and other high energy nuclei (HZE ions). Solar energetic particles consist primarily of protons accelerated by the Sun to high energies via proximity to solar flares and coronal mass ejections. They are one of the most important barriers standing in the way of plans for interplanetary travel by crewed spacecraft.