Observation of Neutrinos at Super-Kamiokande Observatory
... and sends the data to 6 data-consolidation/eventtriggering computers. These computers consolidate the data received from the readout computers, search for the physics events over the entire detector, and record event data at a rate of about 12 kHz. Event triggering in large-scale particle physics ex ...
... and sends the data to 6 data-consolidation/eventtriggering computers. These computers consolidate the data received from the readout computers, search for the physics events over the entire detector, and record event data at a rate of about 12 kHz. Event triggering in large-scale particle physics ex ...
Abundances and possible diffusion of elements in M 67 stars⋆
... abundance trend in iron was found between the turn-off point and the red giants (Mucciarelli et al. 2011), possibly indicating that the more massive outer convection zones of more metal-rich stars suppress atomic diffusion. It is now important to find out to what extent such diffusion effects are also v ...
... abundance trend in iron was found between the turn-off point and the red giants (Mucciarelli et al. 2011), possibly indicating that the more massive outer convection zones of more metal-rich stars suppress atomic diffusion. It is now important to find out to what extent such diffusion effects are also v ...
Circum-stellar medium around rotating massive stars at solar
... from the zero-age main sequence up to the end of central carbon burning and cover the main stages of stellar evolution: main sequence, RSG, or WR phase, if any. After carbon is exhausted in the centre of the star, the core evolution becomes so fast that the surface is insensitive to what happens in ...
... from the zero-age main sequence up to the end of central carbon burning and cover the main stages of stellar evolution: main sequence, RSG, or WR phase, if any. After carbon is exhausted in the centre of the star, the core evolution becomes so fast that the surface is insensitive to what happens in ...
A Model for the Universe (6) -
... Space has already been defined as the potentiality (or capability) to exhibit volume, latent volume so to speak. For any volume to exist in the real sense (as compared to the imagining or visualizing of a volume) it must contain something. That is, something must fill the volume, something that is o ...
... Space has already been defined as the potentiality (or capability) to exhibit volume, latent volume so to speak. For any volume to exist in the real sense (as compared to the imagining or visualizing of a volume) it must contain something. That is, something must fill the volume, something that is o ...
Toward $ ab\, initio $ extremely metal poor stars
... Bromm & Lee 2016). The resulting stars should have final masses on the order of a few tens of solar masses. These massive stars rapidly convert hydrogen and helium into heavier elements in just a few million years (Schaerer 2002) and explode as core-collapse supernovae (Heger & Woosley 2002). The pr ...
... Bromm & Lee 2016). The resulting stars should have final masses on the order of a few tens of solar masses. These massive stars rapidly convert hydrogen and helium into heavier elements in just a few million years (Schaerer 2002) and explode as core-collapse supernovae (Heger & Woosley 2002). The pr ...
Summary of dynamics of the regular heptagon: N =7
... The number of ‘distinct’ star polygons for {N} is the number of integers less than N/2 – which we call ‘HalfN’ and write as 〈N/2〉. So for a regular N-gon, the ‘maximal’ star polygon is {N, 〈N/2〉}. (Some authors would also allow the ‘boundary’ cases such as {14,0} and {14,7} – which are isolated poin ...
... The number of ‘distinct’ star polygons for {N} is the number of integers less than N/2 – which we call ‘HalfN’ and write as 〈N/2〉. So for a regular N-gon, the ‘maximal’ star polygon is {N, 〈N/2〉}. (Some authors would also allow the ‘boundary’ cases such as {14,0} and {14,7} – which are isolated poin ...
arXiv:astro-ph/0701792v1 29 Jan 2007
... sphere itself and the background dark matter, the sphere will inevitably collapse. So such instability is mainly affected by the ”external” fluctuations. In another words, the equilibrious sphere will always keep in equilibrium unless there is additional mass from the outside added into the system. ...
... sphere itself and the background dark matter, the sphere will inevitably collapse. So such instability is mainly affected by the ”external” fluctuations. In another words, the equilibrious sphere will always keep in equilibrium unless there is additional mass from the outside added into the system. ...
The ages of pre-main-sequence stars
... star. We present a number of accreting protostellar tracks that can be used to determine age if the initial conditions can be determined and the underlying accretion rate has been constant in the past. Because of the balance established between the Kelvin±Helmholtz, contraction time-scale and the ac ...
... star. We present a number of accreting protostellar tracks that can be used to determine age if the initial conditions can be determined and the underlying accretion rate has been constant in the past. Because of the balance established between the Kelvin±Helmholtz, contraction time-scale and the ac ...
The Be/X-ray transient 4U 0115+ 63/V635 Cassiopeiae
... contribution from a disc, implying that the measured reddening is (almost) purely interstellar. The intrinsic colour of a B0V star is (B − V )0 = −0.26 (Wegner 1994) and therefore the measured (B −V ) = 1.39 implies a reddening E(B − V ) = 1.65 ± 0.08. Using the relationship E(U −B) = E(B −V )[0.69+ ...
... contribution from a disc, implying that the measured reddening is (almost) purely interstellar. The intrinsic colour of a B0V star is (B − V )0 = −0.26 (Wegner 1994) and therefore the measured (B −V ) = 1.39 implies a reddening E(B − V ) = 1.65 ± 0.08. Using the relationship E(U −B) = E(B −V )[0.69+ ...
Highligh in Physics 2005
... The paradigm of accretion has had a major impact on a variety of phenomena in astrophysics; in particular, it has often been applied to the context of proto-stellar disks. We have studied the role of the disk self-gravity on the properties of accretion disks and found that this role may help explain ...
... The paradigm of accretion has had a major impact on a variety of phenomena in astrophysics; in particular, it has often been applied to the context of proto-stellar disks. We have studied the role of the disk self-gravity on the properties of accretion disks and found that this role may help explain ...
Stellar Relaxation Times
... center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number density of clouds is lower, it’s not 1016 times lower! The masses of these clouds are therefore high enough to scatter stars out of their ...
... center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number density of clouds is lower, it’s not 1016 times lower! The masses of these clouds are therefore high enough to scatter stars out of their ...
Chapter 12: The Life Cycle of Stars
... Protostar to Main-sequence Star • Protostar contracts and heats until core temperature is sufficient for hydrogen fusion. • Contraction ends when energy released by hydrogen fusion balances energy radiated from surface. • Takes 50 million years for star like Sun from birth to reach the main se ...
... Protostar to Main-sequence Star • Protostar contracts and heats until core temperature is sufficient for hydrogen fusion. • Contraction ends when energy released by hydrogen fusion balances energy radiated from surface. • Takes 50 million years for star like Sun from birth to reach the main se ...
Nuclear structure studies in the xenon and radon
... [Blau2006]. Therefore the masses of very exotic nuclei, i.e. nuclei far away from the valley of stability with a very short half-life, are in general not very well known and sometimes only extrapolated values exist. In nature these nuclei are mainly produced in stellar reactions under extreme condit ...
... [Blau2006]. Therefore the masses of very exotic nuclei, i.e. nuclei far away from the valley of stability with a very short half-life, are in general not very well known and sometimes only extrapolated values exist. In nature these nuclei are mainly produced in stellar reactions under extreme condit ...
stars - KIAS
... detached binary system, and later have undergone fast evolution during a rapid mass-transfer phase when the former massive and rapidly evolving component overfills it’s Roche lobe and mass-transfer has ...
... detached binary system, and later have undergone fast evolution during a rapid mass-transfer phase when the former massive and rapidly evolving component overfills it’s Roche lobe and mass-transfer has ...
Project 9: Stellar Spectra: Temperature
... depends on the availability of electrons to move to higher energies and on atomic factors, namely the likelihood of absorption in the presence of a passing photon. The efficiencies depend critically on temperature and can be calculated from theory or measured in the labo ...
... depends on the availability of electrons to move to higher energies and on atomic factors, namely the likelihood of absorption in the presence of a passing photon. The efficiencies depend critically on temperature and can be calculated from theory or measured in the labo ...
The evolution of dwarf galaxy satellites with different dark matter
... numerical strategy that in the past has only been attempted for simulations of galaxies in clusters ( Dubinski (1999); Mastropietro et al. (2005)). In this approach, known as the ”replacement technique”, cosmological subhalos are replaced with high resolution models of dwarf galaxies within the orig ...
... numerical strategy that in the past has only been attempted for simulations of galaxies in clusters ( Dubinski (1999); Mastropietro et al. (2005)). In this approach, known as the ”replacement technique”, cosmological subhalos are replaced with high resolution models of dwarf galaxies within the orig ...
masses of star clusters in the nuclei of bulgeless spiral galaxies
... that an observed galaxy spectrum can be represented by the convolution of one or several stellar templates with a certain broadening function, often approximated as a Gaussian. The line width in the template spectra represents both the intrinsic width of the stellar photospheric lines and the instru ...
... that an observed galaxy spectrum can be represented by the convolution of one or several stellar templates with a certain broadening function, often approximated as a Gaussian. The line width in the template spectra represents both the intrinsic width of the stellar photospheric lines and the instru ...
The chemical composition of IK Pegasi
... The Kurucz & Pevtremann (1975) and Kurucz (1988, private communication) line lists were used to identify absorption lines which appeared to be unblended (i.e. more than 95 per cent in the absorption feature was due to only one line). This process was complicated by the moderately high value of v sin ...
... The Kurucz & Pevtremann (1975) and Kurucz (1988, private communication) line lists were used to identify absorption lines which appeared to be unblended (i.e. more than 95 per cent in the absorption feature was due to only one line). This process was complicated by the moderately high value of v sin ...
Overview spherical accretion
... Transform the fluid equations to spherical coordinates (use expression for r in spherical coordinates (BT eq. 1B-46)) and write u=vr, and take u>0 inward: ...
... Transform the fluid equations to spherical coordinates (use expression for r in spherical coordinates (BT eq. 1B-46)) and write u=vr, and take u>0 inward: ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.