The Chemical Composition of the Local Interstellar Dust
... abundance reference: Sun, local F & G stars, B stars Sun: + star that can be studied best + independent abundances from different indicators - 4.56 Gyr old, representative for present-day ISM? F&G stars: + differential abundances relative to Sun + increased number statistics - difficult age determin ...
... abundance reference: Sun, local F & G stars, B stars Sun: + star that can be studied best + independent abundances from different indicators - 4.56 Gyr old, representative for present-day ISM? F&G stars: + differential abundances relative to Sun + increased number statistics - difficult age determin ...
ppt - Astronomy & Physics
... The space between stars is filled by extremely low density gas called the Interstellar Medium (ISM) ...
... The space between stars is filled by extremely low density gas called the Interstellar Medium (ISM) ...
SPA 302: THE EVOLUTION OF STARS LECTURE 1: BASICS OF
... Man's intrigues about the stars has over the years grown immensely and crystallized into a solid physical theory that provides scientists with a frame of reference on which to interpret many aspects about our Universe. Stars- the hot spherical balls of burning gas that light up the night sky- come i ...
... Man's intrigues about the stars has over the years grown immensely and crystallized into a solid physical theory that provides scientists with a frame of reference on which to interpret many aspects about our Universe. Stars- the hot spherical balls of burning gas that light up the night sky- come i ...
VISIT TO NORMAN LOCKYER OBSERVATORY IN SIDMOUTH
... Virgo, in the south-east after sunset this month, is not one of the most prominent constellations, containing only one bright star, Spica, but is one of the largest and is very rewarding for those with "rich field" telescopes capable of seeing the many galaxies that lie within its boundaries. Spica ...
... Virgo, in the south-east after sunset this month, is not one of the most prominent constellations, containing only one bright star, Spica, but is one of the largest and is very rewarding for those with "rich field" telescopes capable of seeing the many galaxies that lie within its boundaries. Spica ...
8.1 Stars
... The area with the largest mass starts to pull more mass in. The matter pulled in has excess energy which causes the central ball of material to begin to spin. Extremely high pressures build up inside the ball, which in turn causes the tightly packed atoms to heat up. As the temperature climbs, the ...
... The area with the largest mass starts to pull more mass in. The matter pulled in has excess energy which causes the central ball of material to begin to spin. Extremely high pressures build up inside the ball, which in turn causes the tightly packed atoms to heat up. As the temperature climbs, the ...
ASTR2050 Spring 2005 •
... However, we can write this in terms of the period in a way valid for both stars! See Kutner Eq.5.20 and typo! ...
... However, we can write this in terms of the period in a way valid for both stars! See Kutner Eq.5.20 and typo! ...
2.1 Introduction
... 1.0 in Figure 2.8 have values of MV which span 10 magnitudes, or a factor of 10 000! From eq. 2.15 we understand this to be a consequence of their different sizes; evidently, the radii of such stars span a range of two orders of magnitude. For this reason, stars above the main sequence are termed gi ...
... 1.0 in Figure 2.8 have values of MV which span 10 magnitudes, or a factor of 10 000! From eq. 2.15 we understand this to be a consequence of their different sizes; evidently, the radii of such stars span a range of two orders of magnitude. For this reason, stars above the main sequence are termed gi ...
Constellations - Sierra Star Gazers
... has the distinction of being one of the largest and brightest stars in the known galaxy. While too far for a good parallax distance calculation, Mu Cephei is thought to be about 2400 light years away. With a radius 1,650 times larger than our Sun’s, if placed in the center of our solar system the su ...
... has the distinction of being one of the largest and brightest stars in the known galaxy. While too far for a good parallax distance calculation, Mu Cephei is thought to be about 2400 light years away. With a radius 1,650 times larger than our Sun’s, if placed in the center of our solar system the su ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... Students will learn how to interpret observational characteristics of stars in terms of the underlying physical parameters You should gain an understanding of how stars of different mass evolve, and what end products are produced Students should learn what causes planetary nebulae and supernovae You ...
... Students will learn how to interpret observational characteristics of stars in terms of the underlying physical parameters You should gain an understanding of how stars of different mass evolve, and what end products are produced Students should learn what causes planetary nebulae and supernovae You ...
File
... Stars are giant balls of burning ___________ Stars produce energy via nuclear reactions = fusion of _______________ ________________…form elements! Stars are classified by: 1. ...
... Stars are giant balls of burning ___________ Stars produce energy via nuclear reactions = fusion of _______________ ________________…form elements! Stars are classified by: 1. ...
Stars: from Adolescence to Old Age
... • Each time through the cycle, the star creates new heavier elements from the ash of fusion reactions in the previous cycle 12 April 2005 ...
... • Each time through the cycle, the star creates new heavier elements from the ash of fusion reactions in the previous cycle 12 April 2005 ...
Coming Home - Marcia Bartusiak
... comparatively young, bluish stars surrounding a central bulge of old, red stars; but the disk is now much bigger, and it has kinks in it. The new Milky Way still has spi ral arms, but the arms are studded with giant clouds of molecular gas, inside of which astronomers can at last see massive stars ...
... comparatively young, bluish stars surrounding a central bulge of old, red stars; but the disk is now much bigger, and it has kinks in it. The new Milky Way still has spi ral arms, but the arms are studded with giant clouds of molecular gas, inside of which astronomers can at last see massive stars ...
The colour-magnitude diagram
... Hipparcos classified the naked-eye stars according to their apparent brightness, from 1st magnitude – brightest ones – to 6th – faintest ones Eye sensitivity follows a logarithmic law To stick as much as possible to Hipparcos system, astronomers defined the apparent magnitude of a star: ...
... Hipparcos classified the naked-eye stars according to their apparent brightness, from 1st magnitude – brightest ones – to 6th – faintest ones Eye sensitivity follows a logarithmic law To stick as much as possible to Hipparcos system, astronomers defined the apparent magnitude of a star: ...
Bluffing your way in Astronomy: Taurus
... software. they will reveal over two hundred. The faint haze around the stars appears as a beautiful blue mist in photographs. Older astronomy books say this is a wispy remnant of the molecular cloud in which they were born. However astronomers now think the stars in the Pleiades are at least 100 mil ...
... software. they will reveal over two hundred. The faint haze around the stars appears as a beautiful blue mist in photographs. Older astronomy books say this is a wispy remnant of the molecular cloud in which they were born. However astronomers now think the stars in the Pleiades are at least 100 mil ...
The Components of a Spiral Galaxy
... • spheroids have shapes largely supported by velocity dispersion." • Conventional theoretical 'wisdom' : disks form at the center of dark matter halos as a consequence of angular momentum conservation during the dissipational collapse of gas (Fall & Efstathiou 1980) , spheroids result predominantl ...
... • spheroids have shapes largely supported by velocity dispersion." • Conventional theoretical 'wisdom' : disks form at the center of dark matter halos as a consequence of angular momentum conservation during the dissipational collapse of gas (Fall & Efstathiou 1980) , spheroids result predominantl ...
What is a Star?
... – Rods distinguish shades of color while cones distinguish color in general. – Cones do not work well with low light, so one is not easily able to distinguish between colors of stars. ...
... – Rods distinguish shades of color while cones distinguish color in general. – Cones do not work well with low light, so one is not easily able to distinguish between colors of stars. ...
STEPHAN`S QUINTET
... Stephan's Quintet in the constellation Pegasus is al grouping of five galaxies of which four form the first compact galaxy group ever discovered. The group was discovered by Édouard Stephan in 1877 at Marseilles Observatory. These galaxies are of interest because of their violent collisions. Four of ...
... Stephan's Quintet in the constellation Pegasus is al grouping of five galaxies of which four form the first compact galaxy group ever discovered. The group was discovered by Édouard Stephan in 1877 at Marseilles Observatory. These galaxies are of interest because of their violent collisions. Four of ...
Stellar Evolution: the Death of Stars
... collapses and most of its matter is ejected into space at high speeds • The luminosity of the star increases suddenly by a factor of around 108 during this explosion, producing a supernova • The matter ejected from the supernova, moving at supersonic speeds through interstellar gases and dust, glows ...
... collapses and most of its matter is ejected into space at high speeds • The luminosity of the star increases suddenly by a factor of around 108 during this explosion, producing a supernova • The matter ejected from the supernova, moving at supersonic speeds through interstellar gases and dust, glows ...
Luminosity Classes
... The width of the absorption lines in a star’s spectrum indicates its density. The thinner the line the less the density. Supergiants & Giants are the least dense. In general the less dense a star is the more luminous it will be (because it has more surface area). Luminosity and the thickness of the ...
... The width of the absorption lines in a star’s spectrum indicates its density. The thinner the line the less the density. Supergiants & Giants are the least dense. In general the less dense a star is the more luminous it will be (because it has more surface area). Luminosity and the thickness of the ...
Chapter 20: Stellar Evolution: The Death of Stars PowerPoint
... • Luminosity increases by a factor of 108 – As bright as an entire galaxy – > 99% of energy is in the form of neutrinos ...
... • Luminosity increases by a factor of 108 – As bright as an entire galaxy – > 99% of energy is in the form of neutrinos ...
Chapter 15
... – The process continues as long as there are enough large stars and gas to propagate the star formation process – Differential rotation of the galaxy then spreads the stars out into a spiral arm – The random nature of the triggering star formation should give a spiral galaxy a ragged look and this i ...
... – The process continues as long as there are enough large stars and gas to propagate the star formation process – Differential rotation of the galaxy then spreads the stars out into a spiral arm – The random nature of the triggering star formation should give a spiral galaxy a ragged look and this i ...
Astronomy 401 Lecture 8 Spiral Galaxies II 1 The Tully
... The classic spiral galaxy is called a grand design spiral, with two symmetric and well-defined arms. Others have more than two arms, or arms that appear fragmented. Galaxies without well-defined arms that can be traced over a large angular distance are called flocculent spirals. Grand design: ∼ 10% ...
... The classic spiral galaxy is called a grand design spiral, with two symmetric and well-defined arms. Others have more than two arms, or arms that appear fragmented. Galaxies without well-defined arms that can be traced over a large angular distance are called flocculent spirals. Grand design: ∼ 10% ...
Class II Supernova
... Stars with anywhere from 3-9 solar masses have hydrogen in their core. When the hydrogen combines with the helium, it produces thermal energy. This is how the star is maintained. When the star runs out or stops producing hydrogen the thermal energy doesn’t maintain the star anymore. ...
... Stars with anywhere from 3-9 solar masses have hydrogen in their core. When the hydrogen combines with the helium, it produces thermal energy. This is how the star is maintained. When the star runs out or stops producing hydrogen the thermal energy doesn’t maintain the star anymore. ...
Lecture 29 Our Galaxy: "Milky Way"
... Galactic Rotation Galactic material must be in some kind of orbit around the center, or gravity would pull everything into the center! • Rotation of Galaxy is real tough to measure (can't actually see rotation in our lifetime), but get a rough idea as follows, mainly from doppler radial velocities: ...
... Galactic Rotation Galactic material must be in some kind of orbit around the center, or gravity would pull everything into the center! • Rotation of Galaxy is real tough to measure (can't actually see rotation in our lifetime), but get a rough idea as follows, mainly from doppler radial velocities: ...
Test 1, Feb. 2, 2016 - Brock physics
... 35. Type II supernova occurs (a) in a white dwarf-star binary system when the mass transfer pushes the mass of the white dwarf above the maximum value it can have. (b) when a regular star is swallowed by a black hole. (c) when a large mass stars explodes. (d) in a pulsar-star binary system when the ...
... 35. Type II supernova occurs (a) in a white dwarf-star binary system when the mass transfer pushes the mass of the white dwarf above the maximum value it can have. (b) when a regular star is swallowed by a black hole. (c) when a large mass stars explodes. (d) in a pulsar-star binary system when the ...
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.