DTU_9e_ch12
... Sketches of and light curves for three eclipsing binaries are shown. The phase denotes the fraction of the orbital period from one primary minimum to the next. (a) Algol, also known as β Persei, is a semidetached binary. The deep eclipse occurs when the giant star (right) blocks the light from the s ...
... Sketches of and light curves for three eclipsing binaries are shown. The phase denotes the fraction of the orbital period from one primary minimum to the next. (a) Algol, also known as β Persei, is a semidetached binary. The deep eclipse occurs when the giant star (right) blocks the light from the s ...
What could it be?: the nature of dark matter
... •Observation: Galaxy clusters are emiting a lot of X-rays •Explanation: Inside cluster: presence of hot ionized gas at several million degrees •Those clouds would contain roughly 10 times more mass than the cluster galaxies total visible mass •The kinetic energy of gas molecule is very large: virial ...
... •Observation: Galaxy clusters are emiting a lot of X-rays •Explanation: Inside cluster: presence of hot ionized gas at several million degrees •Those clouds would contain roughly 10 times more mass than the cluster galaxies total visible mass •The kinetic energy of gas molecule is very large: virial ...
2_ISM - UCT Astronomy Department
... •Reminder: Extinction caused by both scattering and absorption • Absorption: radiant energy transformed into heat, re-radiated at IR wavelengths corresponding to temperatures of dust particles reduced intensity and reddening of colour • Scattering: the direction of light changed as f(λ), leading t ...
... •Reminder: Extinction caused by both scattering and absorption • Absorption: radiant energy transformed into heat, re-radiated at IR wavelengths corresponding to temperatures of dust particles reduced intensity and reddening of colour • Scattering: the direction of light changed as f(λ), leading t ...
Document
... a burst is seen with total energy release of ~1042 erg; these last for ~ an hour and are likely produced by unstable c-burning in deeper layers. ...
... a burst is seen with total energy release of ~1042 erg; these last for ~ an hour and are likely produced by unstable c-burning in deeper layers. ...
Exam #2 Solutions
... Either hotter main sequence stars or cooler giants. The hotter main sequence stars are mostly B and A stars with temperatures around 15,000 K and luminosities between 50 and 5,000 solar luminosities, The cooler giant stars are mostly K and M giants with temperatures around 5,000 K to 3,000K an ...
... Either hotter main sequence stars or cooler giants. The hotter main sequence stars are mostly B and A stars with temperatures around 15,000 K and luminosities between 50 and 5,000 solar luminosities, The cooler giant stars are mostly K and M giants with temperatures around 5,000 K to 3,000K an ...
talk
... to 800 m (cf. Klaas et al. 2001) • M(H2) = 0.8 L(CO1-0) (Downes & Solomon 1998); assume CO3-2/1-0=0.5 (our data) • Calculate gas to dust ratio in central beam only (CO much more sensitive than continuum per unit mass) • Average gas/dust ratio = 120 +/- 30 ...
... to 800 m (cf. Klaas et al. 2001) • M(H2) = 0.8 L(CO1-0) (Downes & Solomon 1998); assume CO3-2/1-0=0.5 (our data) • Calculate gas to dust ratio in central beam only (CO much more sensitive than continuum per unit mass) • Average gas/dust ratio = 120 +/- 30 ...
STA Binary star model
... Attach a power pack to the motor and adjust the supply to turn the motor slowly (use a supply of less than 2 V d.c.). Use another retort stand to hold the light sensor level with the stars about 1 metre away from the model. Plug the sensor into the datalogger. Change the sampling rate to 50 samples/ ...
... Attach a power pack to the motor and adjust the supply to turn the motor slowly (use a supply of less than 2 V d.c.). Use another retort stand to hold the light sensor level with the stars about 1 metre away from the model. Plug the sensor into the datalogger. Change the sampling rate to 50 samples/ ...
The Spatially-Resolved Scaling Law of Star Formation
... • If, after the nova, it does not shed all the mass it gained, it will continue to accrete mass until it novas again. • If this process continues (accretion, nova, accretion, nova, etc.) such that the WD continues to gain mass, once it has a mass of 1.4Msun, the core will collapse, carbon fusion wil ...
... • If, after the nova, it does not shed all the mass it gained, it will continue to accrete mass until it novas again. • If this process continues (accretion, nova, accretion, nova, etc.) such that the WD continues to gain mass, once it has a mass of 1.4Msun, the core will collapse, carbon fusion wil ...
Sun and Other Stars Notes
... -luminosity class considers density of __________________________ which determines between a bright giant and a supergiant -What are binary-star systems? -two stars that are part of the same solar system we can see them __________________ -Why are eclipsing binaries helpful in studying star features ...
... -luminosity class considers density of __________________________ which determines between a bright giant and a supergiant -What are binary-star systems? -two stars that are part of the same solar system we can see them __________________ -Why are eclipsing binaries helpful in studying star features ...
Document
... Radius of the star turning into a red giant is increasing due to the great increase in luminosity being provided by the fusion occurring in a shell around the core. ...
... Radius of the star turning into a red giant is increasing due to the great increase in luminosity being provided by the fusion occurring in a shell around the core. ...
The formation of the Solar System
... nebula has to cool enough for dust formation to start • Planetesimal formation and growth then can begin • A planetary system does not have unlimited time. As the young star develops, it produces a strong stellar wind that would carry away into space the dust that has not formed into large planetesi ...
... nebula has to cool enough for dust formation to start • Planetesimal formation and growth then can begin • A planetary system does not have unlimited time. As the young star develops, it produces a strong stellar wind that would carry away into space the dust that has not formed into large planetesi ...
Lecture 13 Local group chapter 4 of S+G
... Andromeda), a smaller spiral M33 and lots of (>35 galaxies), most of which are dwarf ellipticals and irregulars with low mass; most are satellites of MW, M31 or M33 The gravitational interaction between these systems is complex but the local group is apparently bound. Major advantages – close and br ...
... Andromeda), a smaller spiral M33 and lots of (>35 galaxies), most of which are dwarf ellipticals and irregulars with low mass; most are satellites of MW, M31 or M33 The gravitational interaction between these systems is complex but the local group is apparently bound. Major advantages – close and br ...
Exploring the Helium Reionization Era
... Exploring the Helium Reionization Era In Big Bang cosmology, the universe began as a hot, dense, gas fireball. Due to its extreme initial temperature, charged particles (ions) within the gas were not bound together into neutral atoms, but freely streamed outward with other subatomic particles as th ...
... Exploring the Helium Reionization Era In Big Bang cosmology, the universe began as a hot, dense, gas fireball. Due to its extreme initial temperature, charged particles (ions) within the gas were not bound together into neutral atoms, but freely streamed outward with other subatomic particles as th ...
Stars - WhatisOutThere
... its own gravity. The stars force of gravity is always causing the star to collapse. The gravity is a balance of hot gas and radiation coming from inside the star. This is called hydrostatic support. A star gives off light by nuclear burning in the stars core. ...
... its own gravity. The stars force of gravity is always causing the star to collapse. The gravity is a balance of hot gas and radiation coming from inside the star. This is called hydrostatic support. A star gives off light by nuclear burning in the stars core. ...
The HR Diagram - Faculty Web Pages
... squeeze the gas all down to a single point, and radiation pressure, which wants to blast all the gas out to infinity. These two opposite forces balance out in a process called Hydrostatic Equilibrium, and keep the gas at a stable, fairly constant size. The radiation itself is due to the fusion of pr ...
... squeeze the gas all down to a single point, and radiation pressure, which wants to blast all the gas out to infinity. These two opposite forces balance out in a process called Hydrostatic Equilibrium, and keep the gas at a stable, fairly constant size. The radiation itself is due to the fusion of pr ...
Galactic Neighborhood and (Chandra-enabled) X-ray Astrophysics Q. Daniel Wang
... • Stable and low non-X-ray background – Particularly important for studying large-scale diffuse X-ray emission. ...
... • Stable and low non-X-ray background – Particularly important for studying large-scale diffuse X-ray emission. ...
Letter to the Editor The formation of bipolar planetary nebulae
... But the morphology of both images is much more bipolar than the ones from run A. At a time of 507 years after the end of the AGB, the stellar effective temperature is 226 000 K. 4. Discussion Both models are still in their early evolutionary stages and one should therefore be careful drawing far rea ...
... But the morphology of both images is much more bipolar than the ones from run A. At a time of 507 years after the end of the AGB, the stellar effective temperature is 226 000 K. 4. Discussion Both models are still in their early evolutionary stages and one should therefore be careful drawing far rea ...
EarthComm_c1s9
... understand when and how these events occur. Not only are these nebulae interesting, but they also show scientists what the fate of our solar system will be billions of years from now. What would happen if there were a supernova explosion in our stellar neighborhood some time in the future? Depending ...
... understand when and how these events occur. Not only are these nebulae interesting, but they also show scientists what the fate of our solar system will be billions of years from now. What would happen if there were a supernova explosion in our stellar neighborhood some time in the future? Depending ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.