Interstellar Medium (ISM) Interstellar Extinction Star Formation
... M ~ 106 Msun, R ~ 10 pc star clusters …on large scales, down to: Molecular cloud cores M ~ few Solar masses R ~ 0.1 pc one or a few stars (From P. Armitage) ...
... M ~ 106 Msun, R ~ 10 pc star clusters …on large scales, down to: Molecular cloud cores M ~ few Solar masses R ~ 0.1 pc one or a few stars (From P. Armitage) ...
The Evolutionary Status of Be Stars in Clusters and in the Galactic
... a luminosity class is performed by analyzing the effects of gravity in the stellar spectrum. In an oblate star, gravity is much higher in the poles than in the equator, and hence the luminosity class also depends on the inclination angle. Taking into account both effects, a rapidly rotating star see ...
... a luminosity class is performed by analyzing the effects of gravity in the stellar spectrum. In an oblate star, gravity is much higher in the poles than in the equator, and hence the luminosity class also depends on the inclination angle. Taking into account both effects, a rapidly rotating star see ...
Instruments and Science Programs - California State University
... the stellar evolutionary link between the central stars of planetary nebulae and white dwarf stars. These stellar variability searches are easy to schedule. Over 300 candidate stars are on my target list, enough for decades of work. They’re all over the sky, so one could observe many on any clear ni ...
... the stellar evolutionary link between the central stars of planetary nebulae and white dwarf stars. These stellar variability searches are easy to schedule. Over 300 candidate stars are on my target list, enough for decades of work. They’re all over the sky, so one could observe many on any clear ni ...
Blackbody radiation Temperature of stars
... Statistical mechanics, Boltzmann distribution, equipartition law Cavity radiation, Rayleigh-Jeans classical formula ...
... Statistical mechanics, Boltzmann distribution, equipartition law Cavity radiation, Rayleigh-Jeans classical formula ...
Lesson Planner Beyond our solar system.indd
... they understand that the stars are still there, but they cannot be seen during the day due to the vast amount of light from the Sun. At night, the contrast between starlight and the surrounding sky is sufficient to enable the stars to stand out and be seen. However, light pollution can obscure starli ...
... they understand that the stars are still there, but they cannot be seen during the day due to the vast amount of light from the Sun. At night, the contrast between starlight and the surrounding sky is sufficient to enable the stars to stand out and be seen. However, light pollution can obscure starli ...
Stellar Temperatures
... • Vega-based magnitudes: the star α Lyr is assigned m = 0 • AB-magnitudes: m = 0 is assigned 3.63 × 10-20 ergs/cm2/s/Hz (i.e., m = -2.5 log Fν – 48.60), regardless of wavelength • ST-magnitudes: m = 0 is assigned 3.63 × 10-9 ergs/cm2/s/Å (i.e., m = -2.5 log Fλ – 21.10), regardless of wavelength I ...
... • Vega-based magnitudes: the star α Lyr is assigned m = 0 • AB-magnitudes: m = 0 is assigned 3.63 × 10-20 ergs/cm2/s/Hz (i.e., m = -2.5 log Fν – 48.60), regardless of wavelength • ST-magnitudes: m = 0 is assigned 3.63 × 10-9 ergs/cm2/s/Å (i.e., m = -2.5 log Fλ – 21.10), regardless of wavelength I ...
Document
... Unlike stars, clouds of gas do not pass through density waves unscathed Gas clouds are compressed as they slow down Gas clouds rear-end one another Both cause cloud collapse & forming new stars, especially hot, luminous (OB) stars. These light up the spiral arms. ...
... Unlike stars, clouds of gas do not pass through density waves unscathed Gas clouds are compressed as they slow down Gas clouds rear-end one another Both cause cloud collapse & forming new stars, especially hot, luminous (OB) stars. These light up the spiral arms. ...
Supernovae and compact objects
... very closely in a binary system. If they are sufficiently close, they will emit gravitational radiation as they orbit, which will remove energy from the orbit and cause them to eventually collide and merge. This is referred to as the double-degenerate scenario, since it involves two degenerate stars ...
... very closely in a binary system. If they are sufficiently close, they will emit gravitational radiation as they orbit, which will remove energy from the orbit and cause them to eventually collide and merge. This is referred to as the double-degenerate scenario, since it involves two degenerate stars ...
Spin-Orbit Angles as a Probe to Orbital Evolution
... to Teff <6150 K. Tides are dissipated more effectively when there is an outer convective layer (Zahn 1977). Winn et al. (2010) have postulated that tides have changed the distribution in spin-orbit angles of planets orbiting stars <6150K, but left the distribution intact for systems >6350K. It is stil ...
... to Teff <6150 K. Tides are dissipated more effectively when there is an outer convective layer (Zahn 1977). Winn et al. (2010) have postulated that tides have changed the distribution in spin-orbit angles of planets orbiting stars <6150K, but left the distribution intact for systems >6350K. It is stil ...
Document
... Unlike stars, clouds of gas do not pass through density waves unscathed Gas clouds are compressed as they slow down Gas clouds rear-end one another Both cause cloud collapse & forming new stars, especially hot, luminous (OB) stars. These light up the spiral arms. ...
... Unlike stars, clouds of gas do not pass through density waves unscathed Gas clouds are compressed as they slow down Gas clouds rear-end one another Both cause cloud collapse & forming new stars, especially hot, luminous (OB) stars. These light up the spiral arms. ...
BIG BANG –Webquest
... GO to the following site: http://www.windows2universe.org/the_universe/AllStarTop.html a. Click “The Sun.” How much time does light take to travel from the sun to Earth? ____________________ b. Hit the back button. Click “Sirius A” (the BRIGHTEST star in the sky!) How much time does light take to tr ...
... GO to the following site: http://www.windows2universe.org/the_universe/AllStarTop.html a. Click “The Sun.” How much time does light take to travel from the sun to Earth? ____________________ b. Hit the back button. Click “Sirius A” (the BRIGHTEST star in the sky!) How much time does light take to tr ...
Radio Microwave Infrared Visible Speed in Vacuum 3.00 x 108 m s
... Warm Objects Terrain Clouds Meteorology Communication GPS Cell Phones Microwaves ...
... Warm Objects Terrain Clouds Meteorology Communication GPS Cell Phones Microwaves ...
AND STARS! The Sun s Source of Energy E= m c
... Survey Question Suppose you could magically inject, all at once, a large amount of energy into the core of the Sun. What would happen? 1) The Sun would contract as the core heated up. 2) The Sun would contract as the energy became gravitational potential energy and find new equilibrium with the gra ...
... Survey Question Suppose you could magically inject, all at once, a large amount of energy into the core of the Sun. What would happen? 1) The Sun would contract as the core heated up. 2) The Sun would contract as the energy became gravitational potential energy and find new equilibrium with the gra ...
Lecture20
... helium, it has an energy crisis Because the star is small, it cannot ignite the remaining material in its core and so the star collapses and forms a ...
... helium, it has an energy crisis Because the star is small, it cannot ignite the remaining material in its core and so the star collapses and forms a ...
Chapter 6: Terrestrial Planets - Department of Physics and Astronomy
... absolute mag. Apparent + absolute mag -> DISTANCE ...
... absolute mag. Apparent + absolute mag -> DISTANCE ...
Clase-06_Star_Formation - Departamento de Astronomía
... global (or super) winds are also found, powered by energy of starlight, stellar winds and supernovae associated very luminous compact star clusters (up to 108 L) frequently occur (if these objects have a normal IMF, and remain gravitationally bound after the mass loss from massive members is co ...
... global (or super) winds are also found, powered by energy of starlight, stellar winds and supernovae associated very luminous compact star clusters (up to 108 L) frequently occur (if these objects have a normal IMF, and remain gravitationally bound after the mass loss from massive members is co ...
High-mass stars in the Galactic center Quintuplet cluster
... the luminous late-type WN stars (WNL) are an interphase between O stars leaving the main-sequence and WR stars of the carbon sequence (WC), before these massive stars explode as supernova (SN). As shown in the HRD (Fig. 4) the WNL stars in the Quintuplet form a group of relatively cool but very lumi ...
... the luminous late-type WN stars (WNL) are an interphase between O stars leaving the main-sequence and WR stars of the carbon sequence (WC), before these massive stars explode as supernova (SN). As shown in the HRD (Fig. 4) the WNL stars in the Quintuplet form a group of relatively cool but very lumi ...
Interacting binary stars Properties of some binary stars are
... has too much angular momentum to fall directly onto the surface of the other star: Gas forms an accretion disk around the mass gaining star, through which the gas slowly spirals in before being accreted. This occurs if the accreting star does not have a strong magnetic field. ...
... has too much angular momentum to fall directly onto the surface of the other star: Gas forms an accretion disk around the mass gaining star, through which the gas slowly spirals in before being accreted. This occurs if the accreting star does not have a strong magnetic field. ...
Astronomy
... Learning Target: Be able to explain what causes various types of stellar explosions Question of the day: Once you have your test back, use your book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting ...
... Learning Target: Be able to explain what causes various types of stellar explosions Question of the day: Once you have your test back, use your book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting ...
Powerpoint
... a) those heavier than iron, because of supernovae b) iron, formed just before massive stars explode c) odd-numbered nuclei, built with hydrogen fusion d) even-numbered nuclei, built with helium fusion ...
... a) those heavier than iron, because of supernovae b) iron, formed just before massive stars explode c) odd-numbered nuclei, built with hydrogen fusion d) even-numbered nuclei, built with helium fusion ...
The Chemical Composition of Stars in Open Clusters
... able to study clusters at distances of up to 6 kpc or so. Recent work has shown that large-scale abundance gradients are indeed present in the disko I may refer again to the work of Mayor, who found a decrease of the metal abundance by a factor of 2 over a distance of 3 kpc in the radial direction. ...
... able to study clusters at distances of up to 6 kpc or so. Recent work has shown that large-scale abundance gradients are indeed present in the disko I may refer again to the work of Mayor, who found a decrease of the metal abundance by a factor of 2 over a distance of 3 kpc in the radial direction. ...
gravPart2
... • Turn the Sun’s velocity direction (keep amplitude) such that the Sun can fall into the BH at Galactic Centre. How accurate must the aiming be in term of angles in arcsec? Find input values from speed of the Sun, BH mass and distances from literature. • Consider a giant star (of 100solar radii, 1 s ...
... • Turn the Sun’s velocity direction (keep amplitude) such that the Sun can fall into the BH at Galactic Centre. How accurate must the aiming be in term of angles in arcsec? Find input values from speed of the Sun, BH mass and distances from literature. • Consider a giant star (of 100solar radii, 1 s ...
PowerPoint version is here
... How it works! Gravity pushes inward, but the center of the sun in heated by nuclear reactions, making a high pressure that pushes outwards. They balance, and the sun just sits there burning its nuclear fuel. This has gone on for 4.5 billion years and will continue for another 5 billion years. ...
... How it works! Gravity pushes inward, but the center of the sun in heated by nuclear reactions, making a high pressure that pushes outwards. They balance, and the sun just sits there burning its nuclear fuel. This has gone on for 4.5 billion years and will continue for another 5 billion years. ...
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or ""dwarf"" stars.After a star has formed, it generates thermal energy in the dense core region through the nuclear fusion of hydrogen atoms into helium. During this stage of the star's lifetime, it is located along the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and other factors. All main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. The strong dependence of the rate of energy generation in the core on the temperature and pressure helps to sustain this balance. Energy generated at the core makes its way to the surface and is radiated away at the photosphere. The energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.The main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. Stars below about 1.5 times the mass of the Sun (or 1.5 solar masses (M☉)) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. Above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the CNO cycle that produces helium from hydrogen atoms. Main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. Below this mass, stars have cores that are entirely radiative with convective zones near the surface. With decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases, whereas main-sequence stars below 0.4 M☉ undergo convection throughout their mass. When core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.In general, the more massive a star is, the shorter its lifespan on the main sequence. After the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the HR diagram. The behavior of a star now depends on its mass, with stars below 0.23 M☉ becoming white dwarfs directly, whereas stars with up to ten solar masses pass through a red giant stage. More massive stars can explode as a supernova, or collapse directly into a black hole.