2_ISM - UCT Astronomy Department
... shown the importance of dust absorption and scattering, and Rayleigh scattering in the determination of the true size of the Galaxy • distances to object in the Galaxy • mapping distances to other galaxies • determination of the total light, hence luminous matter • apart from being the ingredient in ...
... shown the importance of dust absorption and scattering, and Rayleigh scattering in the determination of the true size of the Galaxy • distances to object in the Galaxy • mapping distances to other galaxies • determination of the total light, hence luminous matter • apart from being the ingredient in ...
A Type II Supernovae Constraint on $\ nu_e $
... [3-5]. Sterile neutrinos are also suggested as dark matter candidates if they have proper mixings with active neutrinos [6]. In this paper we attempt to consider νe -νs mixing in another astrophysical environment–the Type II supernova (hereafter we omit “type II” for simplicity) core. Since there is ...
... [3-5]. Sterile neutrinos are also suggested as dark matter candidates if they have proper mixings with active neutrinos [6]. In this paper we attempt to consider νe -νs mixing in another astrophysical environment–the Type II supernova (hereafter we omit “type II” for simplicity) core. Since there is ...
ch19
... Interstellar matter moves around the galactic center rapidly (shown by the red arrows) and is compressed as it passes through the slow-moving spiral arms (whose motion is shown by the blue arrows). This compression triggers star formation in the interstellar matter, so that new stars appear on the “ ...
... Interstellar matter moves around the galactic center rapidly (shown by the red arrows) and is compressed as it passes through the slow-moving spiral arms (whose motion is shown by the blue arrows). This compression triggers star formation in the interstellar matter, so that new stars appear on the “ ...
Stellar Metamorphosis as Alternative to Nebular Hypothesis
... of tons of star shrapnel known as asteroids, meteorites and small moon-like objects that are undifferentiated. [26] Therefore TYC 8241 2652 is not evidence of star/planet formation but star/planet destruction caused by objects clearing their path for more stable orbits. [27] Mainstream has this proc ...
... of tons of star shrapnel known as asteroids, meteorites and small moon-like objects that are undifferentiated. [26] Therefore TYC 8241 2652 is not evidence of star/planet formation but star/planet destruction caused by objects clearing their path for more stable orbits. [27] Mainstream has this proc ...
PPT Only - Harvard-Smithsonian Center for Astrophysics
... How Much Gas Could Be Pulled Along for the Ride? RBH [arcsec at 500 pc] ...
... How Much Gas Could Be Pulled Along for the Ride? RBH [arcsec at 500 pc] ...
![Cosmic variance in [O/Fe] in the Galactic disk](http://s1.studyres.com/store/data/014331057_1-996ec6eddf93071c5e835624d4620c7e-300x300.png)
Cosmic variance in [O/Fe] in the Galactic disk
... If two metals are produced in the same proportions in supernovae, their abundance ratio in the ISM will remain constant. If they are produced at different sites or with different proportions, they can be used to constrain the chemical enrichment history of a galaxy, even without any explicit referen ...
... If two metals are produced in the same proportions in supernovae, their abundance ratio in the ISM will remain constant. If they are produced at different sites or with different proportions, they can be used to constrain the chemical enrichment history of a galaxy, even without any explicit referen ...
EXPLORING FUNDAMENTAL PHYSICS WITH NEUTRON STARS
... Like for all stars, neutron star masses can be measured when they belong to binary systems, using Kepler’s third law coupled to other orbital data. In particular, double neutron star binaries present additional observable general relativistic effects (post-Keplerian parameters), due to the very stro ...
... Like for all stars, neutron star masses can be measured when they belong to binary systems, using Kepler’s third law coupled to other orbital data. In particular, double neutron star binaries present additional observable general relativistic effects (post-Keplerian parameters), due to the very stro ...
Hubble Diagram Instruction Sheet
... There are two classes of supernovae, Type I and Type II. For this activity we will be using Type Ia supernovae only. Type Ia supernovae are very important in astronomy as they offer the most reliable sources for measuring cosmic distances up to and beyond 1000 mega parsecs (Mpc). A parsec (pc) is a ...
... There are two classes of supernovae, Type I and Type II. For this activity we will be using Type Ia supernovae only. Type Ia supernovae are very important in astronomy as they offer the most reliable sources for measuring cosmic distances up to and beyond 1000 mega parsecs (Mpc). A parsec (pc) is a ...
THE ORION CONSTELLATION the Great Hunter
... known visual binary since 1831, possibly even earlier, when F. G. Struve first measured it. Rigel is surrounded by a shell of expelled gas. The name Rigel comes from an Arabic phrase meaning “the left foot” Rigel marks Orion’s left foot. Rigel is a blue supergiant. It belongs to the spectral type B8 ...
... known visual binary since 1831, possibly even earlier, when F. G. Struve first measured it. Rigel is surrounded by a shell of expelled gas. The name Rigel comes from an Arabic phrase meaning “the left foot” Rigel marks Orion’s left foot. Rigel is a blue supergiant. It belongs to the spectral type B8 ...
Testing - uwyo.edu
... What would happen to a contracting cloud fragment if it were not able to radiate away its thermal energy? A. It would continue contracting, but its temperature would not change. B. Its mass would increase. C. Its internal pressure would increase. ...
... What would happen to a contracting cloud fragment if it were not able to radiate away its thermal energy? A. It would continue contracting, but its temperature would not change. B. Its mass would increase. C. Its internal pressure would increase. ...
east and west encounter at sea
... of that, new voyages were made to the previously discovered places, and its techniques involved orientation by the stars, swells, wind and birds. On the other hand, in the Atlantic during the exploration of the West African coast in the first half of the fifteenth century, and its progress towards t ...
... of that, new voyages were made to the previously discovered places, and its techniques involved orientation by the stars, swells, wind and birds. On the other hand, in the Atlantic during the exploration of the West African coast in the first half of the fifteenth century, and its progress towards t ...
STAR ANALYSER 100 USER MANUAL PATON HAWKSLEY EDUCATION LTD
... It is the science of recording and analysing electromagnetic radiation (eg light) in terms of its wavelength (colour). 2 Why is Spectroscopy so important in Astronomy? Astronomy is rather unusual among the sciences in that it is almost entirely observational rather than experimental. With the rare e ...
... It is the science of recording and analysing electromagnetic radiation (eg light) in terms of its wavelength (colour). 2 Why is Spectroscopy so important in Astronomy? Astronomy is rather unusual among the sciences in that it is almost entirely observational rather than experimental. With the rare e ...
INTERSTELLAR MedLab
... Reflection – dust clouds that reflect (scatter) a star’s light to us Dark – high densities of dust and gas that redden or extinct the light from the stars located behind the cloud. These are also where molecules are likely to be found. During the course of this laboratory exercise, you will study th ...
... Reflection – dust clouds that reflect (scatter) a star’s light to us Dark – high densities of dust and gas that redden or extinct the light from the stars located behind the cloud. These are also where molecules are likely to be found. During the course of this laboratory exercise, you will study th ...
The Chemical Composition of Carbon-Rich, Very Metal
... put forward to account for the moderately metal-poor classical CH stars ([Fe/H]∼ −1.5). These are usually explained by a model involving mass transfer from a carbon-enhanced asymptotic giant branch (AGB) star (one that has since evolved to the white dwarf stage and cannot now be seen) to its lower-m ...
... put forward to account for the moderately metal-poor classical CH stars ([Fe/H]∼ −1.5). These are usually explained by a model involving mass transfer from a carbon-enhanced asymptotic giant branch (AGB) star (one that has since evolved to the white dwarf stage and cannot now be seen) to its lower-m ...
1 Pau Amaro Seoane - modest 15-s
... We present an expression of the external gravitational field of a general ring-like object with the axial and plane symmetries such as annular disks or oval toroids with an arbitrary density distribution. The main term is that of an infinitely thin ring (Fukushima, 2010, Celest. Mech. Dyn. Astron., ...
... We present an expression of the external gravitational field of a general ring-like object with the axial and plane symmetries such as annular disks or oval toroids with an arbitrary density distribution. The main term is that of an infinitely thin ring (Fukushima, 2010, Celest. Mech. Dyn. Astron., ...
Time, quantum and information
... into one helium-4 nucleus is accompanied by a mass loss of 0.71 per cent of the initial masses, or 0.029 u. It is converted into an energy of about 26.2 MeV, including the annihilation energy of the two positrons that are produced, and the energy that is carried away by two electron neutrinos. From ...
... into one helium-4 nucleus is accompanied by a mass loss of 0.71 per cent of the initial masses, or 0.029 u. It is converted into an energy of about 26.2 MeV, including the annihilation energy of the two positrons that are produced, and the energy that is carried away by two electron neutrinos. From ...
The accretion disk paradigm for young stars
... of a number of these objects, now known as YY Ori stars after their prototype, and had noticed the presence of red-displaced, highly variable absorption components in the Balmer lines of these objects, indicating infall velocity of up to 400 km/s. In these spectra the Balmer jump is clearly in emiss ...
... of a number of these objects, now known as YY Ori stars after their prototype, and had noticed the presence of red-displaced, highly variable absorption components in the Balmer lines of these objects, indicating infall velocity of up to 400 km/s. In these spectra the Balmer jump is clearly in emiss ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.