(massive) binary stars
... for single B-type stars. In our analysis, we will benefit from the precisely determined values of the surface gravity (from dynamical mass and radius) and the effective temperature (net result of the Fig. 2 Nitrogen abundance (12 + log[N/H]) vs. the vsini for core hydrogen burning stars. The removed ...
... for single B-type stars. In our analysis, we will benefit from the precisely determined values of the surface gravity (from dynamical mass and radius) and the effective temperature (net result of the Fig. 2 Nitrogen abundance (12 + log[N/H]) vs. the vsini for core hydrogen burning stars. The removed ...
Looking for the siblings of the Sun
... meteorites, the Sun was polluted by a SN of star about 15-25 solar masses within a distance of 0.02-1.6 pc (Looney et al. 2006). - Star cluster where the Sun was born: M ~ 500-3000 ...
... meteorites, the Sun was polluted by a SN of star about 15-25 solar masses within a distance of 0.02-1.6 pc (Looney et al. 2006). - Star cluster where the Sun was born: M ~ 500-3000 ...
Astronomy Unit Notes
... o Ion tail always points away from the sun o Dust tail is left behind in the comets path of travel Asteroid = a large chunk of rock traveling through space. Most, not all, are found in the asteroid belt located between Mars and Jupiter. Meteoroid = a small piece of rock moving through space. Meteo ...
... o Ion tail always points away from the sun o Dust tail is left behind in the comets path of travel Asteroid = a large chunk of rock traveling through space. Most, not all, are found in the asteroid belt located between Mars and Jupiter. Meteoroid = a small piece of rock moving through space. Meteo ...
How are galaxies classified
... Centauri. It can only be seen from the southern hemisphere. The brightest star in the northern hemisphere (other than our sun) is ...
... Centauri. It can only be seen from the southern hemisphere. The brightest star in the northern hemisphere (other than our sun) is ...
Slide sem título - Instituto de Física / UFRJ
... (9.2X1011 g/cm3) to 5X103 MeV/fm3 (9.2X1015 g/cm3). We can see in fig. 1 that both the total mass and radius of the stars are increased by the presence of charge. Fig. 2 shows how much charge these stars can have. Table 1 shows these results for the maximum mass configuration [4]. ...
... (9.2X1011 g/cm3) to 5X103 MeV/fm3 (9.2X1015 g/cm3). We can see in fig. 1 that both the total mass and radius of the stars are increased by the presence of charge. Fig. 2 shows how much charge these stars can have. Table 1 shows these results for the maximum mass configuration [4]. ...
Lecture 26 Pre-Main Sequence Evolution
... Local Star Forming Regions Much of our knowledge of star formation comes from a few nearby regions ...
... Local Star Forming Regions Much of our knowledge of star formation comes from a few nearby regions ...
Planet Mass ~13 M E
... • Contact (K) - the two stars are in contact, usually no clean start/stop of eclipse • Semidetached (SD) - the two stars are near one another, often ellipsoidal in shape, with perhaps Roche lobe overflow • Detached (D) - no influence by one star on the other, usually flat between eclipses • Period i ...
... • Contact (K) - the two stars are in contact, usually no clean start/stop of eclipse • Semidetached (SD) - the two stars are near one another, often ellipsoidal in shape, with perhaps Roche lobe overflow • Detached (D) - no influence by one star on the other, usually flat between eclipses • Period i ...
How the Universe Works: Supernova Video Guide
... they begin to ______________________. 4. Pressure pushes _________________ and gravity pushes _________________. 5. When energy is no longer produced in the core of the star, _________________ crushes the star. The outer layers of the star expand outwards, producing a _______________________. 6. The ...
... they begin to ______________________. 4. Pressure pushes _________________ and gravity pushes _________________. 5. When energy is no longer produced in the core of the star, _________________ crushes the star. The outer layers of the star expand outwards, producing a _______________________. 6. The ...
3. Galactic Dynamics handout 3 Aim: understand equilibrium of
... What are the relevant timescales? Do galaxies evolve along a sequence of equilibria ? [like stars] ? ...
... What are the relevant timescales? Do galaxies evolve along a sequence of equilibria ? [like stars] ? ...
3. Galactic Dynamics handout 3 Aim: understand equilibrium of
... What are the relevant timescales? Do galaxies evolve along a sequence of equilibria ? [like stars] ? ...
... What are the relevant timescales? Do galaxies evolve along a sequence of equilibria ? [like stars] ? ...
Implies dark halo for self-enrichment
... 400 fibres, 2-degree FOV, dual beam, chemical abundances from blue spectra, R ~ 5000, range 3850-4540Å. Membership based on radial velocity (to better than 10 km/s) and the derived values of ...
... 400 fibres, 2-degree FOV, dual beam, chemical abundances from blue spectra, R ~ 5000, range 3850-4540Å. Membership based on radial velocity (to better than 10 km/s) and the derived values of ...
The Milky Way
... The Cycle Doesn’t Last • Mass locked up in the end products of stellar evolution – WD, NS, and BH ...
... The Cycle Doesn’t Last • Mass locked up in the end products of stellar evolution – WD, NS, and BH ...
01-Introduction
... The gas supply to the individual depends on their location in the cluster and the competition within the cluster and within the system. Observation and theory then demonstrate principles of mass segregation. These studies of the dynamical evolution, with remarkable spatial resolution provided by the ...
... The gas supply to the individual depends on their location in the cluster and the competition within the cluster and within the system. Observation and theory then demonstrate principles of mass segregation. These studies of the dynamical evolution, with remarkable spatial resolution provided by the ...
Xtra_credit_MC_chapt_10−12_2014.txt Xtra_credit_MC_chapt_10
... 3) As a result of gravity the helium core of a red giant continues to collapse until something happens in the core of the (1 solar mass) star to stop the collapse? a) ignition of the hydrogen (in the shell just outside the helium core) in a "hydrogen flash" b) ignition of helium fusion (in the heliu ...
... 3) As a result of gravity the helium core of a red giant continues to collapse until something happens in the core of the (1 solar mass) star to stop the collapse? a) ignition of the hydrogen (in the shell just outside the helium core) in a "hydrogen flash" b) ignition of helium fusion (in the heliu ...
22_SN1987a
... • A shock wave rebounds through the outer layers of the star: some of the neutrons fly out through the ejecta and make heavy elements by 56Fe + Nn 56+NX • The core continues to collapse: it either halts as a stable neutron star or becomes a black hole depending upon the mass remaining in the core ...
... • A shock wave rebounds through the outer layers of the star: some of the neutrons fly out through the ejecta and make heavy elements by 56Fe + Nn 56+NX • The core continues to collapse: it either halts as a stable neutron star or becomes a black hole depending upon the mass remaining in the core ...
ppt - University of Cambridge
... Cepheid Variable Stars • Cepheids are special stars because they blink, what’s more they blink at a rate that is precisely related to their brightness. – If we can measure the rate that they are blinking then we can infer how bright they are. – Then we compare how bright they look to us and how bri ...
... Cepheid Variable Stars • Cepheids are special stars because they blink, what’s more they blink at a rate that is precisely related to their brightness. – If we can measure the rate that they are blinking then we can infer how bright they are. – Then we compare how bright they look to us and how bri ...
A Brief History of History
... under gravity formed the first galaxies and that the stars inside these clouds were formed later by the same process on a smaller scale. Stars come next A star is a ball of super-hot gas balanced between the twin tendencies to collapse under its own gravity, and the outward pressure of radiation ene ...
... under gravity formed the first galaxies and that the stars inside these clouds were formed later by the same process on a smaller scale. Stars come next A star is a ball of super-hot gas balanced between the twin tendencies to collapse under its own gravity, and the outward pressure of radiation ene ...
Notes 4, p. 1-3
... ⊲ In a non-equilibrium state, there is not enough outward force to oppose the gravitational collapse so the star begins to contract ⊲ For the star to contract, gravitational potential energy must be lost; in this case it goes into heating the star at a smaller radius (keeping the star shining) ⊲ The ...
... ⊲ In a non-equilibrium state, there is not enough outward force to oppose the gravitational collapse so the star begins to contract ⊲ For the star to contract, gravitational potential energy must be lost; in this case it goes into heating the star at a smaller radius (keeping the star shining) ⊲ The ...
Methods of Energy Transport There are 3 methods for energy
... To decide whether convection occurs in a star, begin by considering a blob of material with volume V in pressure equilibrium with its surroundings. Initially, both the blob and its surroundings have temperature T1 and density ρ1 . Now suppose the blob’s temperature is perturbed, such that its new te ...
... To decide whether convection occurs in a star, begin by considering a blob of material with volume V in pressure equilibrium with its surroundings. Initially, both the blob and its surroundings have temperature T1 and density ρ1 . Now suppose the blob’s temperature is perturbed, such that its new te ...
The Evolution of the Universe and the formation of Black Holes
... sufficiently familiar with them, but invests vast resources in order for that to change. It is speculated that there is around 10 million civilizations similar or different to ours in each galaxy, which contains several billion stars. If these civilizations are much more advance than ours, which can ...
... sufficiently familiar with them, but invests vast resources in order for that to change. It is speculated that there is around 10 million civilizations similar or different to ours in each galaxy, which contains several billion stars. If these civilizations are much more advance than ours, which can ...
Internet Space Scavenger Hunt
... 42.The inner planets of our solar system are ___________, _____________, ___________, and ______________. Mercury, Venus, Earth, Mars 43.The __________, which is located between Mars and Jupiter, contains thousands of irregular fragments. Asteroid belt 44.______________ are made of frozen lumps of g ...
... 42.The inner planets of our solar system are ___________, _____________, ___________, and ______________. Mercury, Venus, Earth, Mars 43.The __________, which is located between Mars and Jupiter, contains thousands of irregular fragments. Asteroid belt 44.______________ are made of frozen lumps of g ...
Lecture102102 - FSU High Energy Physics
... The light put out by stars contains absorption lines ...
... The light put out by stars contains absorption lines ...
Salpeter Mass Function
... Comments on the Salpeter IMF What is the origin of the IMF? Most important unsolved problem in star formation. Many theories but no consensus. Observationally, known that dense cores in molecular clouds have a power-law mass function rather similar to the IMF. So the IMF may be determined in part b ...
... Comments on the Salpeter IMF What is the origin of the IMF? Most important unsolved problem in star formation. Many theories but no consensus. Observationally, known that dense cores in molecular clouds have a power-law mass function rather similar to the IMF. So the IMF may be determined in part b ...
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.