Physics- HSC- Module 9.7 Astrophysics
... During the late 19th and early 20th centuries, astronomers obtained spectra and parallax distances for many stars, a powerful tool was discovered for classifying and understanding stars. Around 1911-13, Enjar Hertzsprung and Henry Norris Russell independently found that stars could be divided into t ...
... During the late 19th and early 20th centuries, astronomers obtained spectra and parallax distances for many stars, a powerful tool was discovered for classifying and understanding stars. Around 1911-13, Enjar Hertzsprung and Henry Norris Russell independently found that stars could be divided into t ...
key - Scioly.org
... 32. What is the Chandrasekhar limit, in solar masses? [1] 33. Neutron stars are to white dwarfs as the ...
... 32. What is the Chandrasekhar limit, in solar masses? [1] 33. Neutron stars are to white dwarfs as the ...
Recipe for a Star
... supernova. The explosion is so powerful that it can briefly outshine an entire galaxy. It is the most violent and spectacular explosion in the universe. While the core explosion occurs in about one second, the massive-star supernova may continue to shine for weeks or months. Massive-star supernovae ...
... supernova. The explosion is so powerful that it can briefly outshine an entire galaxy. It is the most violent and spectacular explosion in the universe. While the core explosion occurs in about one second, the massive-star supernova may continue to shine for weeks or months. Massive-star supernovae ...
Measuring the Stars Section 29.2
... While stars are in the main sequence, they are fusing hydrogen in their cores. As stars evolve off the main sequence, they begin to fuse helium in their cores and burn hydrogen around the core edges. ...
... While stars are in the main sequence, they are fusing hydrogen in their cores. As stars evolve off the main sequence, they begin to fuse helium in their cores and burn hydrogen around the core edges. ...
Science and the Universe
... • From our location within the Galaxy, we cannot see through its far rim because the space between stars is not empty, but contains (an extremely sparse distribution of) interstellar dust or gas which absorbs visible light • The interstellar gas and dust are believed to be the raw material for futur ...
... • From our location within the Galaxy, we cannot see through its far rim because the space between stars is not empty, but contains (an extremely sparse distribution of) interstellar dust or gas which absorbs visible light • The interstellar gas and dust are believed to be the raw material for futur ...
Planet Building Part 4
... rare, though we know they are common (in our SS and in others). • To solve the Jovian problem, astronomers have posited that Jovian formation was from direct collapse. – In other words, the condensation and accretion ...
... rare, though we know they are common (in our SS and in others). • To solve the Jovian problem, astronomers have posited that Jovian formation was from direct collapse. – In other words, the condensation and accretion ...
15.1 Introduction
... and UV spectra are dominated by strong, broad emission lines instead of the narrow absorption lines that are typical of ‘normal’ stars (Figure 15.3). The emission lines are so strong that they were first noticed as early as 1867 by... Charles Wolf and Georges Rayet (!) using the 40 cm Foucault teles ...
... and UV spectra are dominated by strong, broad emission lines instead of the narrow absorption lines that are typical of ‘normal’ stars (Figure 15.3). The emission lines are so strong that they were first noticed as early as 1867 by... Charles Wolf and Georges Rayet (!) using the 40 cm Foucault teles ...
B LOG - Science Centre
... The Dipper is part of a much larger star pattern, the constellation Ursa Major (Greater Bear) although it had a variety of meanings in many cultures. Most common is that of a bear or a ladle/dipper used for scooping water. Other representations include a plough, an ox or horse pulling a plough and t ...
... The Dipper is part of a much larger star pattern, the constellation Ursa Major (Greater Bear) although it had a variety of meanings in many cultures. Most common is that of a bear or a ladle/dipper used for scooping water. Other representations include a plough, an ox or horse pulling a plough and t ...
Procedurally Generating an Artificial Galaxy
... While you have the ability to roll a die, spin a wheel or toss a coin to generate random numbers, computers are restricted to so-called pseudorandom number generators (PRNG's). Their basic principal is simple: an input number, called a seed, is transformed into a seemingly random output number by an ...
... While you have the ability to roll a die, spin a wheel or toss a coin to generate random numbers, computers are restricted to so-called pseudorandom number generators (PRNG's). Their basic principal is simple: an input number, called a seed, is transformed into a seemingly random output number by an ...
![[C ii] 157 μm Emission in a Five-component Interstellar](http://s1.studyres.com/store/data/019898103_1-04a729a979ed8700f387bc0fbfcce724-300x300.png)
[C ii] 157 μm Emission in a Five-component Interstellar
... cd type galaxy located at the distance of 11.6Mpc, while NGC 628 is an SA(s)c type galaxy located at 7.2Mpc (Kennicutt et al. 2003). At this distance, an aperture size of 12″ corresponds to a physical size of 500–600 pc. On this scale it is very likely to have multiple H II regions and dense PDRs ...
... cd type galaxy located at the distance of 11.6Mpc, while NGC 628 is an SA(s)c type galaxy located at 7.2Mpc (Kennicutt et al. 2003). At this distance, an aperture size of 12″ corresponds to a physical size of 500–600 pc. On this scale it is very likely to have multiple H II regions and dense PDRs ...
van der Wel et al., 2004, ApJ, 602, L5 - ST-ECF
... We present deep VLT spectra of early-type galaxies at z ≈ 1 in the Chandra Deep Field–South, from which we derive velocity dispersions. Together with structural parameters from Hubble Space Telescope imaging, we can study the fundamental plane for field early-type galaxies at that epoch. We determin ...
... We present deep VLT spectra of early-type galaxies at z ≈ 1 in the Chandra Deep Field–South, from which we derive velocity dispersions. Together with structural parameters from Hubble Space Telescope imaging, we can study the fundamental plane for field early-type galaxies at that epoch. We determin ...
GALAXY FORMATION AND CLUSTER FORMATION Richard B
... mostly within the first few Gyr. They must therefore have been more compact than typical present-day irregular or spiral galaxies, since a higher star formation rate requires a higher mean density (Larson 1977). Typical irregular or spiral galaxies also do not make clusters as massive as typical glo ...
... mostly within the first few Gyr. They must therefore have been more compact than typical present-day irregular or spiral galaxies, since a higher star formation rate requires a higher mean density (Larson 1977). Typical irregular or spiral galaxies also do not make clusters as massive as typical glo ...
the origin of the hubble sequence - Yale Astronomy
... The timescale for gravitational instability or swing amplification effects is approximately τ ∼ c/πGμ, and thus it depends on both the velocity dispersion c and the surface density μ of the gas. Two possible limiting cases have been considered by Larson (1988, 1992) in discussing the implied paramete ...
... The timescale for gravitational instability or swing amplification effects is approximately τ ∼ c/πGμ, and thus it depends on both the velocity dispersion c and the surface density μ of the gas. Two possible limiting cases have been considered by Larson (1988, 1992) in discussing the implied paramete ...
26.2 Stars - Clinton Public Schools
... measure their distances directly. Astronomers are able to observe stars from two different positions–opposite sides of Earth’s orbit. Nearby stars appear to move against the moredistant background stars. ...
... measure their distances directly. Astronomers are able to observe stars from two different positions–opposite sides of Earth’s orbit. Nearby stars appear to move against the moredistant background stars. ...
6 The mysterious universe
... releases vast amounts of energy. enough to be seen with the naked eye. The collapse continues under the influence of gravity, forming visible globules in the nebula cloud. As the globules collapse further, the formation of any original gas A quick glance around the night sky shows us that cloud is a ...
... releases vast amounts of energy. enough to be seen with the naked eye. The collapse continues under the influence of gravity, forming visible globules in the nebula cloud. As the globules collapse further, the formation of any original gas A quick glance around the night sky shows us that cloud is a ...
The Sun and Stars
... Earth. The Hubble Space Telescope is a school-bus-size telescope that orbits Earth every 97 minutes at an altitude of 353 miles and a speed of about 17,500 miles per hour. The Hubble Space Telescope (HST) transmits images and data from space to computers on Earth. In fact, HST sends enough data back ...
... Earth. The Hubble Space Telescope is a school-bus-size telescope that orbits Earth every 97 minutes at an altitude of 353 miles and a speed of about 17,500 miles per hour. The Hubble Space Telescope (HST) transmits images and data from space to computers on Earth. In fact, HST sends enough data back ...
2900 K micrometers T
... absorption lines in the same locations as A7IV, which are also the same locations as the EMISSION lines in the hydrogen comparison spectrum). Other stars have additional elements too, because they have more absorption lines that are not accounted for by hydrogen. ...
... absorption lines in the same locations as A7IV, which are also the same locations as the EMISSION lines in the hydrogen comparison spectrum). Other stars have additional elements too, because they have more absorption lines that are not accounted for by hydrogen. ...
Formation of z~6 Quasars from Hierarchical Galaxy Mergers
... ¥Need to grow a BH up to 109 Msun in less than 800 million years. ¥1. Pair instability PopIII - BH ~102 Msun ¥2. Hot, dense clumps of gas collapse to form ~106 Msun ¥3. ~20 Msun BHs from direct collapse of self-gravitating gas due to global instabilities. ¥In simulation - it is necessary for galaxy ...
... ¥Need to grow a BH up to 109 Msun in less than 800 million years. ¥1. Pair instability PopIII - BH ~102 Msun ¥2. Hot, dense clumps of gas collapse to form ~106 Msun ¥3. ~20 Msun BHs from direct collapse of self-gravitating gas due to global instabilities. ¥In simulation - it is necessary for galaxy ...
The surface composition of Beta Pictoris
... has prompted King and Patten (1992) to suggest that β Pic is a λ Boo star. We note that the HST GHRS data analyzed by Lanz and Hubeny (1995) also rule out a low metallicity, and that their own evaluation of Geneva indices leads to a normal rather than subsolar iron abundance. Why does the signature ...
... has prompted King and Patten (1992) to suggest that β Pic is a λ Boo star. We note that the HST GHRS data analyzed by Lanz and Hubeny (1995) also rule out a low metallicity, and that their own evaluation of Geneva indices leads to a normal rather than subsolar iron abundance. Why does the signature ...
Chapter 26.2 notes
... measure their distances directly. Astronomers are able to observe stars from two different positions–opposite sides of Earth’s orbit. Nearby stars appear to move against the moredistant background stars. ...
... measure their distances directly. Astronomers are able to observe stars from two different positions–opposite sides of Earth’s orbit. Nearby stars appear to move against the moredistant background stars. ...
HD 140283: A Star in the Solar Neighborhood that Formed Shortly
... treated, apart from the small adjustment to [Fe/H] = −2.3 described above, but the effect of this neglect on derived ages is very small. At low metallicities, the locations of the turnoff and subgiant portions of isochrones in the HRD depend most strongly on the absolute abundance of oxygen (e.g., V ...
... treated, apart from the small adjustment to [Fe/H] = −2.3 described above, but the effect of this neglect on derived ages is very small. At low metallicities, the locations of the turnoff and subgiant portions of isochrones in the HRD depend most strongly on the absolute abundance of oxygen (e.g., V ...
Formation of elliptical galaxies
... •Good agreement of both with intermediate mass giant elliptical galaxies (see also Cox et al. 2006) •Disk merger remnants, as well as ULIRGS, can follow the Fundamental Plane and the MBH-relation (Robertson et al. 2005; Springel et al. 2005) •Mergers trigger strong central and extended starbursts ...
... •Good agreement of both with intermediate mass giant elliptical galaxies (see also Cox et al. 2006) •Disk merger remnants, as well as ULIRGS, can follow the Fundamental Plane and the MBH-relation (Robertson et al. 2005; Springel et al. 2005) •Mergers trigger strong central and extended starbursts ...
Amazon S3
... star formation is much higher than average. Astronomers have observed galaxies in which the rate is 100 times higher than the Milky Way's. We know this to be a short-lived stage because if it had been going on for more than hundred million years the galaxy would have run out of the gas from which th ...
... star formation is much higher than average. Astronomers have observed galaxies in which the rate is 100 times higher than the Milky Way's. We know this to be a short-lived stage because if it had been going on for more than hundred million years the galaxy would have run out of the gas from which th ...
PSU/TCfA search for planets around evolved stars
... detect the reflex motion of a star due to planetary companion. Radial velocity method, however is not sensitive only to the motion of a star around the center of mass of star-planet system. Changes in line shapes arising from stellar atmospheric motion (caused by non-radial pulsation or inhomogeneou ...
... detect the reflex motion of a star due to planetary companion. Radial velocity method, however is not sensitive only to the motion of a star around the center of mass of star-planet system. Changes in line shapes arising from stellar atmospheric motion (caused by non-radial pulsation or inhomogeneou ...
Life as a Low
... clusters show star becomes larger, redder, and more luminous after its time on the main sequence is over. ...
... clusters show star becomes larger, redder, and more luminous after its time on the main sequence is over. ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.