The Birth, Life, and Death of Stars
... What is the raw material for making stars and where did it come from? What forces of nature contribute to energy generation in stars? How and where did the chemical elements form? ? How long do stars live? How will our Sun die? How do massive stars explode? ? What are the remnants of such stellar ex ...
... What is the raw material for making stars and where did it come from? What forces of nature contribute to energy generation in stars? How and where did the chemical elements form? ? How long do stars live? How will our Sun die? How do massive stars explode? ? What are the remnants of such stellar ex ...
Chapter 9 “The Family of Stars “
... Blurring by the atmosphere smears images to 1 second of arc. ...
... Blurring by the atmosphere smears images to 1 second of arc. ...
Which Constellation is Which?
... You probably know some constellations. The Big Dipper looks like a giant pot with a long handle. Orion is named after a great hunter. You can see his belt, marked by three bright stars. Constellations are imaginary pictures in the sky. The stars look like they are all the same distance away. That’s ...
... You probably know some constellations. The Big Dipper looks like a giant pot with a long handle. Orion is named after a great hunter. You can see his belt, marked by three bright stars. Constellations are imaginary pictures in the sky. The stars look like they are all the same distance away. That’s ...
Hertzsprung-Russell Diagrams and Distance to Stars
... to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than a dim star that’s much closer. To overcome this problem, scientists began to look at stars ...
... to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than a dim star that’s much closer. To overcome this problem, scientists began to look at stars ...
Colour - Magnitude Diagram for M 45
... Colour - Magnitude Diagram for M 45 (Pleiades) Introduction The Pleiades is a relatively close open cluster. The six or seven stars visible to the naked eye form a tight grouping of stars (an asterism) near the even closer Hyades cluster. They are easily visible in the winter sky in the northern hem ...
... Colour - Magnitude Diagram for M 45 (Pleiades) Introduction The Pleiades is a relatively close open cluster. The six or seven stars visible to the naked eye form a tight grouping of stars (an asterism) near the even closer Hyades cluster. They are easily visible in the winter sky in the northern hem ...
WORD - hrsbstaff.ednet.ns.ca
... c. the structure and evolution of the earth's crust. d. everything in the universe that lies above Earth's atmosphere. 02. Which of the following terms would not be associated with astronomy? a. horoscope b. telescope c. astrolabe d. celestial sphere 03. A planet is an object which a. occurs only in ...
... c. the structure and evolution of the earth's crust. d. everything in the universe that lies above Earth's atmosphere. 02. Which of the following terms would not be associated with astronomy? a. horoscope b. telescope c. astrolabe d. celestial sphere 03. A planet is an object which a. occurs only in ...
Chapter 10 Hertzsprung-Russel Diagrams and Distance to Stars
... to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than a dim star that’s much closer. To overcome this problem, scientists began to look at stars ...
... to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than a dim star that’s much closer. To overcome this problem, scientists began to look at stars ...
Stars
... When deuterium and tritium atoms, both hydrogen isotopes, fuse together inside a star, helium is produced. Heavier elements are produced when a star becomes a red giant. Only a supernova can produce elements heavier than iron, such as silver, gold and uranium. ...
... When deuterium and tritium atoms, both hydrogen isotopes, fuse together inside a star, helium is produced. Heavier elements are produced when a star becomes a red giant. Only a supernova can produce elements heavier than iron, such as silver, gold and uranium. ...
Star Formation - Leslie Looney
... •! But if H2 can stick to the dust grains, shouldn’t larger molecules stick too? In fact, we see water (H2O), ammonia (NH3), methane (CH4), and methanol (CH3OH) frozen to the dust grains. •! Hey, that’s the most important bioelements (H, O, N, and C) on dust grains! •! Mayo Greenberg and co-workers ...
... •! But if H2 can stick to the dust grains, shouldn’t larger molecules stick too? In fact, we see water (H2O), ammonia (NH3), methane (CH4), and methanol (CH3OH) frozen to the dust grains. •! Hey, that’s the most important bioelements (H, O, N, and C) on dust grains! •! Mayo Greenberg and co-workers ...
Luminosity - UCF Physics
... What the “computers” did was sift through literally 100’s of thousands of stellar spectra. Established a classification scheme based on Hydrogen lines…. The types were alphabetical….letters were assigned in declining strength of the H-lines ...
... What the “computers” did was sift through literally 100’s of thousands of stellar spectra. Established a classification scheme based on Hydrogen lines…. The types were alphabetical….letters were assigned in declining strength of the H-lines ...
32Brightness
... • Absorption from cooler gases in front of continuum source, where discrete colors are absorbed by atoms – From emission and absorption lines, get composition of objects and also their temperature ...
... • Absorption from cooler gases in front of continuum source, where discrete colors are absorbed by atoms – From emission and absorption lines, get composition of objects and also their temperature ...
Synthetic color-magnitude diagrams: the ingredients
... at time t = 0, no metals were present; hence Z(0) = 0. – The galaxy did not contain any stars at the time of its birth, so that all baryonic matter was in the form of gas. – In addition, we consider the galaxy as a closed system out of which no matter can escape or be added later on by processes o ...
... at time t = 0, no metals were present; hence Z(0) = 0. – The galaxy did not contain any stars at the time of its birth, so that all baryonic matter was in the form of gas. – In addition, we consider the galaxy as a closed system out of which no matter can escape or be added later on by processes o ...
Picture: Alnitak is the left-hand star in Orion`s Belt. Image: NASA
... carbon/oxygen ratios that are typically four to five times higher than those of normal red giants and show little trace of the light metal oxide bands that are the usual red giant hallmark. They resemble S stars in their relative proportion of heavy and light metals, but contain far more carbon in t ...
... carbon/oxygen ratios that are typically four to five times higher than those of normal red giants and show little trace of the light metal oxide bands that are the usual red giant hallmark. They resemble S stars in their relative proportion of heavy and light metals, but contain far more carbon in t ...
Stars, Galaxies, and the Universe
... in it. dust, stars. and gas bound together by gravity. An eclipsing Scientific notation binaryuses is a star powers system of ten in to which writeone very star cannot large orgalaxies be very seen small at times numbers because in shorter other form. starmiddle blocks Spiral appear to have a the bu ...
... in it. dust, stars. and gas bound together by gravity. An eclipsing Scientific notation binaryuses is a star powers system of ten in to which writeone very star cannot large orgalaxies be very seen small at times numbers because in shorter other form. starmiddle blocks Spiral appear to have a the bu ...
Stars I - Astronomy Centre
... around the Sun and rotation of the planet about its own spin axis respectively • Given that angular momentum depends on mass, size of object/orbit and velocity of rotation/revolution, which form contributes most to a planet’s total angular momentum? • More than 99% of Solar System’s mass resides in ...
... around the Sun and rotation of the planet about its own spin axis respectively • Given that angular momentum depends on mass, size of object/orbit and velocity of rotation/revolution, which form contributes most to a planet’s total angular momentum? • More than 99% of Solar System’s mass resides in ...
AST1100 Lecture Notes
... to about 10R⊙ . Giant stars fall in the range between 10R⊙ to about 100R⊙ whereas super giants may have radii of several 100 solar radii. The masses of stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments expla ...
... to about 10R⊙ . Giant stars fall in the range between 10R⊙ to about 100R⊙ whereas super giants may have radii of several 100 solar radii. The masses of stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments expla ...
REVIEWS The formation of the first stars and galaxies Volker Bromm
... few hundred million years after the Big Bang, were identified as the sites where the first stars formed7. Building on this general framework, and relying on the development of efficient new computational tools, the fragmentation properties of primordial gas inside such minihaloes were investigated w ...
... few hundred million years after the Big Bang, were identified as the sites where the first stars formed7. Building on this general framework, and relying on the development of efficient new computational tools, the fragmentation properties of primordial gas inside such minihaloes were investigated w ...
Time From the Perspective of a Particle Physicist
... Traveled 175,000 light years to Earth Passed through Earth ...
... Traveled 175,000 light years to Earth Passed through Earth ...
Chapter 20
... The regions of gas and dust (often called clouds, or “giant molecular clouds”) from which stars are forming are best observed in the infrared and radio regions of the spectrum, because most other forms of radiation (such as optical and ultraviolet) cannot penetrate them. ...
... The regions of gas and dust (often called clouds, or “giant molecular clouds”) from which stars are forming are best observed in the infrared and radio regions of the spectrum, because most other forms of radiation (such as optical and ultraviolet) cannot penetrate them. ...
October 2014 - Hermanus Astronomy
... be, so this is where our simulations come in,” said Celine Boehm from Durham University. “By tuning the strength of the scattering of particles, we change the number of small galaxies, which lets us learn more about the physics of dark matter and how it might interact with other particles in the uni ...
... be, so this is where our simulations come in,” said Celine Boehm from Durham University. “By tuning the strength of the scattering of particles, we change the number of small galaxies, which lets us learn more about the physics of dark matter and how it might interact with other particles in the uni ...
Spectra PowerPoint
... Three types of Spectra Continuous: from glowing solids or very compressed gases, such as the photosphere of the Sun Emission: from hot, glowing gases that are rarefied (not very compressed, such as an emission nebula or features in the solar atmosphere Absorption: a combination spectrum produced b ...
... Three types of Spectra Continuous: from glowing solids or very compressed gases, such as the photosphere of the Sun Emission: from hot, glowing gases that are rarefied (not very compressed, such as an emission nebula or features in the solar atmosphere Absorption: a combination spectrum produced b ...
test - Scioly.org
... 1. Consider an object of .2 solar masses orbiting the Sun. The object’s orbit has a semimajor axis of 6 AU. a. How long is its period in years? b. Consider the points A, B, C, D on the orbit of the object. The arc length from point A to point B is .225 AU. The arc length from point C to D is .556 AU ...
... 1. Consider an object of .2 solar masses orbiting the Sun. The object’s orbit has a semimajor axis of 6 AU. a. How long is its period in years? b. Consider the points A, B, C, D on the orbit of the object. The arc length from point A to point B is .225 AU. The arc length from point C to D is .556 AU ...
The abundance of 26Al-rich planetary systems in the Galaxy
... of 26 Al in the nascent solar system has been that of the nearby supernova (Cameron & Truran 1977). This model stipulates that having reached the end of its evolution and exploding as a supernova, a massive star delivered 26 Al directly into the SPD (Ouellette et al. 2010) or alternatively into the ...
... of 26 Al in the nascent solar system has been that of the nearby supernova (Cameron & Truran 1977). This model stipulates that having reached the end of its evolution and exploding as a supernova, a massive star delivered 26 Al directly into the SPD (Ouellette et al. 2010) or alternatively into the ...
Cosmochemistry from Nanometers to Light- Years A Written by
... Studies of isotopes in chondrites and differentiated (melted) meteorites show that aluminum-26 (26Al) was present when the Solar System formed. Although not abundant (a few parts in 100,000) compared to the stable aluminum isotope (27Al), its half-life is so short (only 730,000 years) that its decay ...
... Studies of isotopes in chondrites and differentiated (melted) meteorites show that aluminum-26 (26Al) was present when the Solar System formed. Although not abundant (a few parts in 100,000) compared to the stable aluminum isotope (27Al), its half-life is so short (only 730,000 years) that its decay ...
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.