CORONAL EVOLUTION OF THE SUN IN TIME: HIGH
... coronal radio and X-ray emissions. The coronal emissions display the largest range of variation in response to the surface magnetic activity level. Whereas starspots may cover a few percent of the photosphere of the most active solar analogs, thus producing a photometric wave with a modulation depth ...
... coronal radio and X-ray emissions. The coronal emissions display the largest range of variation in response to the surface magnetic activity level. Whereas starspots may cover a few percent of the photosphere of the most active solar analogs, thus producing a photometric wave with a modulation depth ...
How Stars Work (Part II)
... Energy of “falling” turned into heat Collapse stops when gravity is balanced by pressure Gravity “bottle” or self-gravity 73% of stars (and all matter in Universe) is Hydrogen Hydrogen is ionized Hot, charges moving ⇒ blackbody ...
... Energy of “falling” turned into heat Collapse stops when gravity is balanced by pressure Gravity “bottle” or self-gravity 73% of stars (and all matter in Universe) is Hydrogen Hydrogen is ionized Hot, charges moving ⇒ blackbody ...
Effects of triple-α and C(α, γ )16 O reaction rates on the supernova
... interactions [30,32]. The reaction rates are taken from the JINA REACLIB compilation [33], where updated nuclear data has been included for charged particle reactions and (n, γ ) cross sections after those of Bao et al. [34]. The finite temperature and density dependences of beta decay and electron ...
... interactions [30,32]. The reaction rates are taken from the JINA REACLIB compilation [33], where updated nuclear data has been included for charged particle reactions and (n, γ ) cross sections after those of Bao et al. [34]. The finite temperature and density dependences of beta decay and electron ...
8-4_Astronomy
... Prominences are huge, looping eruptions of gas, usually near sunspots, that arch out from the photosphere into the outer layers of the Sun’s atmosphere. Solar flares are explosions of hot gas that occur when prominences connect. They shoot from the Sun’s surface releasing tremendous amounts of e ...
... Prominences are huge, looping eruptions of gas, usually near sunspots, that arch out from the photosphere into the outer layers of the Sun’s atmosphere. Solar flares are explosions of hot gas that occur when prominences connect. They shoot from the Sun’s surface releasing tremendous amounts of e ...
The chemical composition of TS 01, the most oxygen
... of a factor 2. Thus the extreme O deficiency of this object is confirmed. The abundances of S and Ar are less than 1/30 of solar. The abundance of He relative to H is 0.089 ± 0.009. Standard models of stellar evolution and nucleosynthesis cannot explain the abundance pattern observed in the nebula. ...
... of a factor 2. Thus the extreme O deficiency of this object is confirmed. The abundances of S and Ar are less than 1/30 of solar. The abundance of He relative to H is 0.089 ± 0.009. Standard models of stellar evolution and nucleosynthesis cannot explain the abundance pattern observed in the nebula. ...
Ascertaining the Core Collapse Supernova Mechanism: An
... where we expect burning actually to occur. On the other hand, when an alpha network is used, burning will occur in the vicinity of the shock, and in this case, partial burning with the release of some nuclear energy is also possible, which may be particularly important for weak shocks. It is this mo ...
... where we expect burning actually to occur. On the other hand, when an alpha network is used, burning will occur in the vicinity of the shock, and in this case, partial burning with the release of some nuclear energy is also possible, which may be particularly important for weak shocks. It is this mo ...
Document
... factors influencing the β-decay lifetime of an unstable nucleus both β- and β+ decay are hampered in the presence of electron or positron degeneracy β- and β+ decays may occur from excited isomeric states maintained in equilibrium with ground state by radiative transitions electron-capture rat ...
... factors influencing the β-decay lifetime of an unstable nucleus both β- and β+ decay are hampered in the presence of electron or positron degeneracy β- and β+ decays may occur from excited isomeric states maintained in equilibrium with ground state by radiative transitions electron-capture rat ...
nuclear reactions in stars: theoretical and experimental
... the availability of experimental data, but in general allows a reliable extrapolation down to stellar energies. The R-matrix theory deals with capture, transfer and elastic scattering on an equal footing. As a general statement, the R-matrix is efficient to describe any process involving continuum s ...
... the availability of experimental data, but in general allows a reliable extrapolation down to stellar energies. The R-matrix theory deals with capture, transfer and elastic scattering on an equal footing. As a general statement, the R-matrix is efficient to describe any process involving continuum s ...
PDF only - at www.arxiv.org.
... The chemistry along the mass loss of Hot Jupiters is generally considered to be simple, consisting mainly of atoms, prevented from forming more complex species by the intense radiation field from their host stars. In order to probe the region where the temperature is low (T < 2000 K), we developed a ...
... The chemistry along the mass loss of Hot Jupiters is generally considered to be simple, consisting mainly of atoms, prevented from forming more complex species by the intense radiation field from their host stars. In order to probe the region where the temperature is low (T < 2000 K), we developed a ...
11.1 Introduction
... constant, then the Jeans mass criterion (eq.11.8) implies that the mass limit for instability decreases dramatically. Any initial density inhomogeneities which may have been present within the cloud will cause individual regions within the GMC to cross the instability threshold independently and col ...
... constant, then the Jeans mass criterion (eq.11.8) implies that the mass limit for instability decreases dramatically. Any initial density inhomogeneities which may have been present within the cloud will cause individual regions within the GMC to cross the instability threshold independently and col ...
Confronting predictions of the galaxy stellar mass function with
... at which the star particle was created. To generate the SED, and thus broad-band photometry, of each galaxy we sum the SEDs of each star particle (weighted by the particle mass). The SED of each star particle is generated using the PEGASE.2 stellar population synthesis (SPS) code (Fioc & RoccaVolmer ...
... at which the star particle was created. To generate the SED, and thus broad-band photometry, of each galaxy we sum the SEDs of each star particle (weighted by the particle mass). The SED of each star particle is generated using the PEGASE.2 stellar population synthesis (SPS) code (Fioc & RoccaVolmer ...
The Death of a Star - hrsbstaff.ednet.ns.ca
... Another method of detecting exoplanets is observing changes in their brightness. It makes sense that when a planet passes between a distant star and an observer on earth the brightness will lessen momentarily. NASA launched a telescope that can measure this change in brightness and use it to calcula ...
... Another method of detecting exoplanets is observing changes in their brightness. It makes sense that when a planet passes between a distant star and an observer on earth the brightness will lessen momentarily. NASA launched a telescope that can measure this change in brightness and use it to calcula ...
L17 SHELL-SHOCKED DIFFUSION MODEL FOR THE LIGHT
... thermal energy. The distinguishing property of the model is that the large “stellar” radius of ∼160 AU required to prevent adiabatic losses is not the true stellar radius, but rather, it is the radius of an opaque, unbound circumstellar envelope, created when ∼10 M, was ejected in the decade before ...
... thermal energy. The distinguishing property of the model is that the large “stellar” radius of ∼160 AU required to prevent adiabatic losses is not the true stellar radius, but rather, it is the radius of an opaque, unbound circumstellar envelope, created when ∼10 M, was ejected in the decade before ...