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... theory they can be seen up to 8000 Mly from Earth. This makes them potentially very interesting as Standard Candles. • Supernovae are divided into various types. Type 1 are thought to be formed by the same kind of event that causes novae. In this case however the White Dwarf collects so much materia ...
... theory they can be seen up to 8000 Mly from Earth. This makes them potentially very interesting as Standard Candles. • Supernovae are divided into various types. Type 1 are thought to be formed by the same kind of event that causes novae. In this case however the White Dwarf collects so much materia ...
Stellar Clusters and Star Formation:
... In simple terms, star formation proceeds in the manner previously discussed – namely a ball of gas collapsed under its own self-gravity until it’s stabilized by sufficient internal pressure. At that point it is a hydrogen fusing main sequence star. However, over the last 25 years we have learned and ...
... In simple terms, star formation proceeds in the manner previously discussed – namely a ball of gas collapsed under its own self-gravity until it’s stabilized by sufficient internal pressure. At that point it is a hydrogen fusing main sequence star. However, over the last 25 years we have learned and ...
Hot Stars With Cool Companions
... fragmentation (Boss & Bodenheimer 1979; Boss 1986; Bate et al. 1995) in which a collapsing cloud of gas fragments into two or more stars. The ratio of masses is set largely by the turbulent power spectrum, density structure, angular momentum, and magnetic field in the pre-stellar core. Low-mass star ...
... fragmentation (Boss & Bodenheimer 1979; Boss 1986; Bate et al. 1995) in which a collapsing cloud of gas fragments into two or more stars. The ratio of masses is set largely by the turbulent power spectrum, density structure, angular momentum, and magnetic field in the pre-stellar core. Low-mass star ...
Test #4 (Ch. 13-16) ASTR 10 You have 1 hour to take the exam, and
... A. Theoretical models of galaxy formation suggest that a galaxy cannot form unless it has at least 10 times as much matter as we see in the Milky Way disk. B. Although dark matter emits no visible light, we have detected its radio emissions. C. The orbital speeds of stars far from the galactic cente ...
... A. Theoretical models of galaxy formation suggest that a galaxy cannot form unless it has at least 10 times as much matter as we see in the Milky Way disk. B. Although dark matter emits no visible light, we have detected its radio emissions. C. The orbital speeds of stars far from the galactic cente ...
Sample Test 22
... 4. This hypothesis was confirmed quantitatively by comparing the amount of rotational energy lost as the object slows down with the amount of energy emitted by the nebula. 5. The Crab pulsar spins so rapidly because it formed relatively recently. Over time it will lose rotational energy, slow down, ...
... 4. This hypothesis was confirmed quantitatively by comparing the amount of rotational energy lost as the object slows down with the amount of energy emitted by the nebula. 5. The Crab pulsar spins so rapidly because it formed relatively recently. Over time it will lose rotational energy, slow down, ...
nuclear fusion atoms
... 8. ______________ _________________ converts matter into energy to create a star's extraordinary heat and light. 9. ____________________ is the universe's most common substance. 10. A big star that explodes might form a super___________ . ...
... 8. ______________ _________________ converts matter into energy to create a star's extraordinary heat and light. 9. ____________________ is the universe's most common substance. 10. A big star that explodes might form a super___________ . ...
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... The integrated spectra of stellar systems, like galaxies and star clusters, contain an extraordinary amount of information, and its analysis can reveal fundamental parameters such as metallicity, age and star formation history. A method that is widely used today is the analysis of the integrated spe ...
... The integrated spectra of stellar systems, like galaxies and star clusters, contain an extraordinary amount of information, and its analysis can reveal fundamental parameters such as metallicity, age and star formation history. A method that is widely used today is the analysis of the integrated spe ...
(massive) binary stars
... confront our results to those of Hunter et al. (2008) and Aerts et al. (2014) to 1) check whether any of the announced correlations are found in our sample, and 2) see whether the differences in the results can be attributed to the effects of tides in binary stars. Star samples, observations, and me ...
... confront our results to those of Hunter et al. (2008) and Aerts et al. (2014) to 1) check whether any of the announced correlations are found in our sample, and 2) see whether the differences in the results can be attributed to the effects of tides in binary stars. Star samples, observations, and me ...
pdf format
... distant parts of the Milky Way and we find that they are moving faster than the Sun, so that their orbital periods are all about the same as the Sun, what does this tell us about the total mass of the Galaxy? Hint in the solar system the more distant planets orbit much more slowly. MGalaxy + Msun = ...
... distant parts of the Milky Way and we find that they are moving faster than the Sun, so that their orbital periods are all about the same as the Sun, what does this tell us about the total mass of the Galaxy? Hint in the solar system the more distant planets orbit much more slowly. MGalaxy + Msun = ...
The Chemical Composition of Stars in Open Clusters
... the solar atmosphere agree so weil with the relative abundances found in meteorites indicates that solar-type stars, i. e. late Fand early G main-sequence stars, have indeed the same atmospheric composition as the material out of which they were formed. Also the composition of most nearby B main-seq ...
... the solar atmosphere agree so weil with the relative abundances found in meteorites indicates that solar-type stars, i. e. late Fand early G main-sequence stars, have indeed the same atmospheric composition as the material out of which they were formed. Also the composition of most nearby B main-seq ...
Lecture 16, PPT version
... • Extraordinarily bright, so can use them to measure distances to galaxies that are very far away: b = L / (4 d2) • Supernovae are the source of all heavy chemical elements! • The heavy chemical elements are produced during the explosion itself, when there is more than enough energy to fuse nuclei ...
... • Extraordinarily bright, so can use them to measure distances to galaxies that are very far away: b = L / (4 d2) • Supernovae are the source of all heavy chemical elements! • The heavy chemical elements are produced during the explosion itself, when there is more than enough energy to fuse nuclei ...
Jeopardy
... •What “fuel” powers the sun? •What process is the fuel used to create energy? •Into what gas is this “fuel” converted? •Where does this occur in the sun? ...
... •What “fuel” powers the sun? •What process is the fuel used to create energy? •Into what gas is this “fuel” converted? •Where does this occur in the sun? ...
Stellar Evolu1on Stars spend most of their lives on the main
... Stars spend most of their lives on the main sequence. Evidence -‐> 90% of stars observable from Earth are main-‐sequence stars. Stellar evolu,on during the main-‐sequence life-‐,me, and during the ...
... Stars spend most of their lives on the main sequence. Evidence -‐> 90% of stars observable from Earth are main-‐sequence stars. Stellar evolu,on during the main-‐sequence life-‐,me, and during the ...
Galaxy may be teeming with small planets
... discover more than 1,000 planets, including more than 500 systems of two or more planets orbiting the same star. What we know best about these planets is their orbital periods. What we would really like to know next is their masses, so we can assess the abundance of planets that have masses similar ...
... discover more than 1,000 planets, including more than 500 systems of two or more planets orbiting the same star. What we know best about these planets is their orbital periods. What we would really like to know next is their masses, so we can assess the abundance of planets that have masses similar ...
2017 New Jersey Science Olympiad Union County College
... Given that the mass of White Dwarf 1 is 1 solar mass and the semimajor axis length of White Dwarf 1 is 1 AU, give the semimajor axis length of White Dwarf 2. (C) Given the radii of White Dwarf 1 being 0.5 solar radii and White Dwarf 2 being 0.2 solar radii, give the densities of the two objects in g ...
... Given that the mass of White Dwarf 1 is 1 solar mass and the semimajor axis length of White Dwarf 1 is 1 AU, give the semimajor axis length of White Dwarf 2. (C) Given the radii of White Dwarf 1 being 0.5 solar radii and White Dwarf 2 being 0.2 solar radii, give the densities of the two objects in g ...
Starbirth - Lincoln-Sudbury Regional High School
... actually “see” inside the cloud. This region has recently been observed with the VLT* at near-infrared wavelengths, which can penetrate the dense dust and reveal the newly born stars. Very young, relatively massive stars are found at the tips of two of the main three pillars, and about a dozen lower ...
... actually “see” inside the cloud. This region has recently been observed with the VLT* at near-infrared wavelengths, which can penetrate the dense dust and reveal the newly born stars. Very young, relatively massive stars are found at the tips of two of the main three pillars, and about a dozen lower ...
Slide 1
... Turn Off - As the hydrogen fuel in a star's core runs out the core begins to collapse due to gravity and the star moves away from the main sequence. At the turn off nearly all the central fuel is gone. Red Giant Branch - When the central fuel is gone, hydrogen starts to burn in an envelope around a ...
... Turn Off - As the hydrogen fuel in a star's core runs out the core begins to collapse due to gravity and the star moves away from the main sequence. At the turn off nearly all the central fuel is gone. Red Giant Branch - When the central fuel is gone, hydrogen starts to burn in an envelope around a ...
ppt
... Wide wavelength coverage emission line spectroscopy gives nebular abundances, ionizing stellar properties (eg. Teff) and virial and wind kinematics Measurements of - or upper limits on - the stellar continuum constrains the IMF Sources expected to cover a range of metallicity from Z ~ 0 to 10-3 ...
... Wide wavelength coverage emission line spectroscopy gives nebular abundances, ionizing stellar properties (eg. Teff) and virial and wind kinematics Measurements of - or upper limits on - the stellar continuum constrains the IMF Sources expected to cover a range of metallicity from Z ~ 0 to 10-3 ...
this PDF file
... In the first attempt only template spectra (with no I2 gas cell inserted) were used for the analysis. However, I2 molecular absorption affects the spectrum up to 660 nm only, so it does not influence 7Li line region. Hence, in the final analysis it was also possible to use the “red” spectra obtained ...
... In the first attempt only template spectra (with no I2 gas cell inserted) were used for the analysis. However, I2 molecular absorption affects the spectrum up to 660 nm only, so it does not influence 7Li line region. Hence, in the final analysis it was also possible to use the “red” spectra obtained ...
Spectral line mapping of the Milky Way
... key ingredients in models of star formation via accretion [27] and to explain the shaping of planetary nebulae [23]. However, the earliest phases of massive star formation may be characterized by short episodes of uncollimated mass-loss [30] Previous studies of Zeeman splitting of OH masers suggest ...
... key ingredients in models of star formation via accretion [27] and to explain the shaping of planetary nebulae [23]. However, the earliest phases of massive star formation may be characterized by short episodes of uncollimated mass-loss [30] Previous studies of Zeeman splitting of OH masers suggest ...
Interstellar Astrophysics Summary notes: Part 5
... Individual collapsing clumps of material (formed in the gas cloud fragmentation) will be relatively cool and several times larger than our Solar System. The pressure is still too low to overcome gravity and the the protostar continues to collapse. As it contracts, some of the gravitational potential ...
... Individual collapsing clumps of material (formed in the gas cloud fragmentation) will be relatively cool and several times larger than our Solar System. The pressure is still too low to overcome gravity and the the protostar continues to collapse. As it contracts, some of the gravitational potential ...
ref star birth - russballard.com
... stars forming near a molecular cloud can set the scene for the next generation of stars. First, the new stars produce strong stellar winds which eat away and compress the edges of the cloud. Some of the stars even supernova. Parts of the cloud then become so dense that a cluster of new massive stars ...
... stars forming near a molecular cloud can set the scene for the next generation of stars. First, the new stars produce strong stellar winds which eat away and compress the edges of the cloud. Some of the stars even supernova. Parts of the cloud then become so dense that a cluster of new massive stars ...
Signatures of the first stars in the 21cm Emission and Absorption
... Properties of first metal-free stars • Central gas cools only to T ≈ 200 K. Molecular hydrogen lines can be collisionally deexcited at density n > 104 cm-3, making the cooling rate independent of density and inhibiting fragmentation. • Jeans mass ≈ 300 Msun . • Accretion rate ≈ cs3/G ≈ 10-3 Msun/yr ...
... Properties of first metal-free stars • Central gas cools only to T ≈ 200 K. Molecular hydrogen lines can be collisionally deexcited at density n > 104 cm-3, making the cooling rate independent of density and inhibiting fragmentation. • Jeans mass ≈ 300 Msun . • Accretion rate ≈ cs3/G ≈ 10-3 Msun/yr ...
The abundance of 26Al-rich planetary systems in the Galaxy
... One of the most distinguished properties of the solar system is the (past) presence of the short-lived radionuclide 26 Al (τ = 1 Myr) in its earliest formed solids (Davis et al. 2014). Magnesium-26 anomalies attributed to the decay of 26 Al were first identified in the calcium-, aluminium-rich inclu ...
... One of the most distinguished properties of the solar system is the (past) presence of the short-lived radionuclide 26 Al (τ = 1 Myr) in its earliest formed solids (Davis et al. 2014). Magnesium-26 anomalies attributed to the decay of 26 Al were first identified in the calcium-, aluminium-rich inclu ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.