Staring Back to Cosmic Dawn - UC-HiPACC
... The Case of the Chaotic Blue Galaxies Ever since Hubble’s first spectacular images of distant galaxies, an enduring puzzle has been why early starforming galaxies look much more irregular and jumbled than nearby blue galaxies. Nearby blue galaxies are relatively smooth. The most beautiful ones are e ...
... The Case of the Chaotic Blue Galaxies Ever since Hubble’s first spectacular images of distant galaxies, an enduring puzzle has been why early starforming galaxies look much more irregular and jumbled than nearby blue galaxies. Nearby blue galaxies are relatively smooth. The most beautiful ones are e ...
DP11 Foundations of Astronomy
... Just as the waves from earthquakes tell us about the Earth's interior as they travel through it, the way that waves travel through the Sun tells us about its interior. Another thing you can observe from the Sun is neutrinos. These are a type of fundamental particle produced in the nuclear fusion rea ...
... Just as the waves from earthquakes tell us about the Earth's interior as they travel through it, the way that waves travel through the Sun tells us about its interior. Another thing you can observe from the Sun is neutrinos. These are a type of fundamental particle produced in the nuclear fusion rea ...
Phys133 Sample MidTerm #2 Covers Chs.10
... D) the instant when hydrogen fusion first begins in the star's core E) when the rate of hydrogen fusion within the star's core is high enough to sustain gravitational equilibrium ...
... D) the instant when hydrogen fusion first begins in the star's core E) when the rate of hydrogen fusion within the star's core is high enough to sustain gravitational equilibrium ...
Distance, Size, and Temperature of a Star
... fuel. Because red dwarf stars only burn a little bit of fuel at a time, they are not very hot compared to other stars. Red dwarf stars are by far the most common type of star in outer space. However, very few stars that you see in the sky are red dwarfs. This is because they are so small and make ve ...
... fuel. Because red dwarf stars only burn a little bit of fuel at a time, they are not very hot compared to other stars. Red dwarf stars are by far the most common type of star in outer space. However, very few stars that you see in the sky are red dwarfs. This is because they are so small and make ve ...
L2 Star formation Part I
... Star formation takes place in cold, dense gas clouds: The molecular clouds. Stars form in groups or clusters. The largest GMC in Orion is about 1000 light years away. Hot young stars (25-50 million year old) ionize their surroundings and are therefore easily visible. ● main characteristics: - molecu ...
... Star formation takes place in cold, dense gas clouds: The molecular clouds. Stars form in groups or clusters. The largest GMC in Orion is about 1000 light years away. Hot young stars (25-50 million year old) ionize their surroundings and are therefore easily visible. ● main characteristics: - molecu ...
Lecture 7
... • Why is the center of the Sun hot? • What is the source of the Sun’s energy? • What are neutrinos & why do we care • How does energy get from the inside to the outside of a star? ...
... • Why is the center of the Sun hot? • What is the source of the Sun’s energy? • What are neutrinos & why do we care • How does energy get from the inside to the outside of a star? ...
Lecture16
... Low pressure: lines are narrow: giant & supergiant stars High pressure: lines are wide: normal stars ...
... Low pressure: lines are narrow: giant & supergiant stars High pressure: lines are wide: normal stars ...
What is a Scientist? - Cockeysville Middle School
... Stars are giant spheres of glowing gases. A star is powered by nuclear fusion. This is a process whereby hydrogen atoms are fused together to create helium atoms. In the process a tremendous amount of energy is given off in the form of electromagnetic waves and heat. There are billions of stars in a ...
... Stars are giant spheres of glowing gases. A star is powered by nuclear fusion. This is a process whereby hydrogen atoms are fused together to create helium atoms. In the process a tremendous amount of energy is given off in the form of electromagnetic waves and heat. There are billions of stars in a ...
The Universe Section 1
... • We learn about stars by studying energy. – Stars produce a full range of electromagnetic radiation, from high-energy X-rays to low-energy radio waves. – Scientists use optical telescopes to study visible light and radio telescopes to study radio waves emitted from astronomical objects. – Earth’s a ...
... • We learn about stars by studying energy. – Stars produce a full range of electromagnetic radiation, from high-energy X-rays to low-energy radio waves. – Scientists use optical telescopes to study visible light and radio telescopes to study radio waves emitted from astronomical objects. – Earth’s a ...
Lecture 9a: More on Star formation and evolution 10/22
... 1. Collapsing Gas Cloud ! Main Sequence Star 2. Brightness depends on Mass 3. Higher Mass also evolve faster - highest mass only “live” a few million years - Sun will “live” about 10 billion years - lower mass stars “live” 100 billion years ...
... 1. Collapsing Gas Cloud ! Main Sequence Star 2. Brightness depends on Mass 3. Higher Mass also evolve faster - highest mass only “live” a few million years - Sun will “live” about 10 billion years - lower mass stars “live” 100 billion years ...
Stars on the HR Diagram
... knowledge astronomers acquire about stars is through mathematical comparison of data derived from the light (radiation) from stars. The Hertzsprung-Russell (HR) Diagram, widely used in astronomy, is a scatter plot with a distribution of data points that describe a relationship between physical aspec ...
... knowledge astronomers acquire about stars is through mathematical comparison of data derived from the light (radiation) from stars. The Hertzsprung-Russell (HR) Diagram, widely used in astronomy, is a scatter plot with a distribution of data points that describe a relationship between physical aspec ...
Chapter 1 Our Place in the Universe
... distance between galaxies is increasing with time. This means that galaxies ( or at least matter) must have been close together in the past. If we go back far enough, all the matter was concentrated in a small radius from which the expansion began. That is called the Big Bang. From the rate of expan ...
... distance between galaxies is increasing with time. This means that galaxies ( or at least matter) must have been close together in the past. If we go back far enough, all the matter was concentrated in a small radius from which the expansion began. That is called the Big Bang. From the rate of expan ...
Physics@Brock - Brock University
... 33. Which of these supernovae emits hydrogen spectral lines? (a) Type Ia. (b) Type II. 34. Type II supernovae are important because (a) the resulting burst of neutrinos keeps the galaxy from collapsing. (b) the elements heavier than iron are synthesized and the elements heavier than helium are dispe ...
... 33. Which of these supernovae emits hydrogen spectral lines? (a) Type Ia. (b) Type II. 34. Type II supernovae are important because (a) the resulting burst of neutrinos keeps the galaxy from collapsing. (b) the elements heavier than iron are synthesized and the elements heavier than helium are dispe ...
Some Examples of Virtual Observatory Enabled Science What Are the Some Distinguishing
... • Some distinction may reflect real, internal physical differences, and some may be simply orientation effects – This is the central thesis of the AGN unification models ...
... • Some distinction may reflect real, internal physical differences, and some may be simply orientation effects – This is the central thesis of the AGN unification models ...
Chapter 27 Quasars, Active Galaxies, and Gamma
... from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like ...
... from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like ...
Photometric Surveys and Variable stars
... lensing. Variable stars are a stated aim for most, but secondary. (High-z SN are the only “variables” mentioned on the LSST front page!) ...
... lensing. Variable stars are a stated aim for most, but secondary. (High-z SN are the only “variables” mentioned on the LSST front page!) ...
1” “Sky-Notes” of the Open University Astronomy Club. June 2005. A
... NGC5669 (11.2) sg. About 1o SE of NGC5676. Barred spiral seen almost edge-on. ...
... NGC5669 (11.2) sg. About 1o SE of NGC5676. Barred spiral seen almost edge-on. ...
TAP 704- 8: The ladder of astronomical distances
... for these models. The Universe according to de Vaucouleurs came out dangerously close to being younger than some of the oldest objects, such as globular star clusters, to be found in it. This was by no means the first time that changes to astronomical distance scales had been suggested. Successive r ...
... for these models. The Universe according to de Vaucouleurs came out dangerously close to being younger than some of the oldest objects, such as globular star clusters, to be found in it. This was by no means the first time that changes to astronomical distance scales had been suggested. Successive r ...
spiral nebulae
... Some of the spiral nebulae seemed clearly to be rotating measurably. That in itself seemed sensible enough, as it would explain why the nebulae were flattened. (Indeed, we now know that they are indeed rotating, just as the Milky Way is.) But there is an important implication: for this rotation to b ...
... Some of the spiral nebulae seemed clearly to be rotating measurably. That in itself seemed sensible enough, as it would explain why the nebulae were flattened. (Indeed, we now know that they are indeed rotating, just as the Milky Way is.) But there is an important implication: for this rotation to b ...
Stellar Evolution
... • As the helium core grows, it compresses. Helium doesn’t fuse to heavier elements for two reasons. (1) with 2 p+ per nucleus, the electric repulsion force is higher than was the case for H-fusion. This means that helium fusion requires a higher temperature than hydrogen fusion -- 100 million K (2) ...
... • As the helium core grows, it compresses. Helium doesn’t fuse to heavier elements for two reasons. (1) with 2 p+ per nucleus, the electric repulsion force is higher than was the case for H-fusion. This means that helium fusion requires a higher temperature than hydrogen fusion -- 100 million K (2) ...
Types of Stars http://space.about.com/od/stars/tp/What-Are
... Black holes are the result of very massive stars collapsing in on themselves due to the massive gravity they create. When the star reaches the end of its main sequence life cycle, the ensuing supernova drives the outer part of the star outward, leaving only the core behind. The core will have become ...
... Black holes are the result of very massive stars collapsing in on themselves due to the massive gravity they create. When the star reaches the end of its main sequence life cycle, the ensuing supernova drives the outer part of the star outward, leaving only the core behind. The core will have become ...
Stars
... all the stars are the same distance, stuck to some sort of Celestial Sphere that rotates through the heavens as the Earth stands still. This conclusion would be very wrong, however. It has taken astronomers thousands of years to realize that stars are different distances from us and that the scale o ...
... all the stars are the same distance, stuck to some sort of Celestial Sphere that rotates through the heavens as the Earth stands still. This conclusion would be very wrong, however. It has taken astronomers thousands of years to realize that stars are different distances from us and that the scale o ...
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.