The secular evolution of the Kuiper belt after a close stellar encounter
... present orbits, long after the dissipation of the initial protoplanetary gas disk. The Nice model seems to provide a acceptable explanation for the formation of the classical and scattered populations, and for the correlation between inclinations and colors (for more detail see Levison et al. (2008) ...
... present orbits, long after the dissipation of the initial protoplanetary gas disk. The Nice model seems to provide a acceptable explanation for the formation of the classical and scattered populations, and for the correlation between inclinations and colors (for more detail see Levison et al. (2008) ...
LesHouches_VanGrootel
... • Global parameters of the star (mass, radius, luminosity, etc.) • Structural and core parameters (Menv, Mcore, core composition, etc) • Constraints for convection, stellar formation & evolution theories... ...
... • Global parameters of the star (mass, radius, luminosity, etc.) • Structural and core parameters (Menv, Mcore, core composition, etc) • Constraints for convection, stellar formation & evolution theories... ...
Presentation (PowerPoint File)
... Simulations of star formation in cores with r r-1.5 Equation of state: isothermal or barotropic above 10^-14 g cm-3 Isothermal collapse results in many small fragments; barotropic collapse in a few. In no case did a massive star form (although simulation ran only until ~ 10% of mass had gone into ...
... Simulations of star formation in cores with r r-1.5 Equation of state: isothermal or barotropic above 10^-14 g cm-3 Isothermal collapse results in many small fragments; barotropic collapse in a few. In no case did a massive star form (although simulation ran only until ~ 10% of mass had gone into ...
ppt
... probably no advantage from multiplexing. Need to select and measure sources from z~3 to the reionization epoch: Ly to z ~ 14 and C IV to z ~ 10.5. The pilot programme will study 5 sources to a limit of mAB ~ 30 (10 hr with JWST in one band). The limiting line flux corresponds to a nebula excited by ...
... probably no advantage from multiplexing. Need to select and measure sources from z~3 to the reionization epoch: Ly to z ~ 14 and C IV to z ~ 10.5. The pilot programme will study 5 sources to a limit of mAB ~ 30 (10 hr with JWST in one band). The limiting line flux corresponds to a nebula excited by ...
Stellar evolution models for Z = 0.0001 to 0.03
... 1993, Claret 1995), we do not parametrize the overshooting length lov in units of the pressure scaleheight HP (which we call the ‘HP prescription’). Instead, we base our treatment on the stability criterion itself, the ‘= prescription’, by incorporating the condition that mixing occurs in a region w ...
... 1993, Claret 1995), we do not parametrize the overshooting length lov in units of the pressure scaleheight HP (which we call the ‘HP prescription’). Instead, we base our treatment on the stability criterion itself, the ‘= prescription’, by incorporating the condition that mixing occurs in a region w ...
Cálculo simplificado
... as the First Point of Aries. But there is a caveat attached. Because of the precession the vernal equinox has shifted westward by almost the full width of a constellation in the last ∼ 2000 years since when the Zodiac signs and constellation were perhaps first identified. As a consequence, the First ...
... as the First Point of Aries. But there is a caveat attached. Because of the precession the vernal equinox has shifted westward by almost the full width of a constellation in the last ∼ 2000 years since when the Zodiac signs and constellation were perhaps first identified. As a consequence, the First ...
Stellar evolution models for Z = 0.0001 to 0.03
... 1993, Claret 1995), we do not parametrize the overshooting length lov in units of the pressure scaleheight HP (which we call the ‘HP prescription’). Instead, we base our treatment on the stability criterion itself, the ‘= prescription’, by incorporating the condition that mixing occurs in a region w ...
... 1993, Claret 1995), we do not parametrize the overshooting length lov in units of the pressure scaleheight HP (which we call the ‘HP prescription’). Instead, we base our treatment on the stability criterion itself, the ‘= prescription’, by incorporating the condition that mixing occurs in a region w ...
Astronomy Standards
... • 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 ...
Volume 11, Number 4 - RASC NB - Royal Astronomical Society of
... through the northern section of our galaxy, it has much less dust, so you can see farther into the deep sky – into galaxy country. The moon will be near first quarter & Venus will be above M45 on Apr. 24, so there will be some great observing opportunities that evening if the weather cooperates. (No ...
... through the northern section of our galaxy, it has much less dust, so you can see farther into the deep sky – into galaxy country. The moon will be near first quarter & Venus will be above M45 on Apr. 24, so there will be some great observing opportunities that evening if the weather cooperates. (No ...
Air Shower Arrays
... having two more post-doctoral fellows. One would work on the data analysis, which would enable us to target interests of the theoretical community in Australia. This would be because Auger will give us data related to AGN source spectra, and intergalactic fields. We would like to ensure that our thr ...
... having two more post-doctoral fellows. One would work on the data analysis, which would enable us to target interests of the theoretical community in Australia. This would be because Auger will give us data related to AGN source spectra, and intergalactic fields. We would like to ensure that our thr ...
ultracam observations of pulsating sdB stars
... = number of lines of nodes passing through the polar axis n: order of the spherical harmonics related to number of nodes along the radial direction ...
... = number of lines of nodes passing through the polar axis n: order of the spherical harmonics related to number of nodes along the radial direction ...
No Slide Title - Laboratory for Atmospheric and Space Physics
... • Observations of this region show shocks, thin “spicules,” and an apparently larger-scale set of convective cells (“super-granulation”). ...
... • Observations of this region show shocks, thin “spicules,” and an apparently larger-scale set of convective cells (“super-granulation”). ...
Available online www.jsaer.com Journal of Scientific and
... seemingly appear white. If the stars are observed via a twin of binoculars, some appear to be different in the light of colours. Many stars appear quite orange in colour and some have a blue/white tint. The colour of a star is a function of its temperature and invariably its size. Stars vary in colo ...
... seemingly appear white. If the stars are observed via a twin of binoculars, some appear to be different in the light of colours. Many stars appear quite orange in colour and some have a blue/white tint. The colour of a star is a function of its temperature and invariably its size. Stars vary in colo ...
Neutron Density and Neutron Source Determination in Barium
... The origin of the large s-process enhancements observed in the classical Barium (Ba 11) stars (Lambert 1985) remains one of the most fundamental challenges in stellar nucleosynthesis theory. An understanding of this phenomenon would lead to an improvement in our knowledge of both s-process systemati ...
... The origin of the large s-process enhancements observed in the classical Barium (Ba 11) stars (Lambert 1985) remains one of the most fundamental challenges in stellar nucleosynthesis theory. An understanding of this phenomenon would lead to an improvement in our knowledge of both s-process systemati ...