Constellations and the Galactic Plane
... are all familiar names to northern hemisphere night sky watchers. There are 88 named constellations, each having numerous stars. This exercise takes you through some of the most recognizable ones in the October-November sky in the Bay Area. The patterns of stars remain the same over the ages. That i ...
... are all familiar names to northern hemisphere night sky watchers. There are 88 named constellations, each having numerous stars. This exercise takes you through some of the most recognizable ones in the October-November sky in the Bay Area. The patterns of stars remain the same over the ages. That i ...
OCR Physics A Refer to the Physics A datasheet for data, formulae
... A binary star system consists of two stars, A and B, rotating about their common centre of mass. Figure 3 shows three absorption lines in the spectra from the binary system measured over a period of time. The diagram is not drawn to ...
... A binary star system consists of two stars, A and B, rotating about their common centre of mass. Figure 3 shows three absorption lines in the spectra from the binary system measured over a period of time. The diagram is not drawn to ...
Day_29
... star remains as white dwarf. They are hot, but not very luminous. Masses 0.6–1.4 M, size like Earth. Density: a ton per teaspoonful! ...
... star remains as white dwarf. They are hot, but not very luminous. Masses 0.6–1.4 M, size like Earth. Density: a ton per teaspoonful! ...
Lecture Nine (Powerpoint format) - Flash
... containing hundreds of thousands of stars in a relatively compact space of a few tens of thousands of light years in diameter. The central densities of the cluster become high enough that stellar collisions can occur. There is some evidence for these stellar collisions in “blue stragglers”. Th ...
... containing hundreds of thousands of stars in a relatively compact space of a few tens of thousands of light years in diameter. The central densities of the cluster become high enough that stellar collisions can occur. There is some evidence for these stellar collisions in “blue stragglers”. Th ...
V: 0
... The student is expected to explore how different wavelengths of the electromagnetic spectrum such as light and radio waves are used to gain information about distances and properties of components in the universe. ...
... The student is expected to explore how different wavelengths of the electromagnetic spectrum such as light and radio waves are used to gain information about distances and properties of components in the universe. ...
PowerPoint
... • Doppler shift– toward (blue) and away (red) • Quantum mechanics– electrons can be wave-like – Electrons around nucleus have certain orbits– defines emission and absorption of each atom – When excited, atoms emit certain lines (like in class)– fingerprint or barcode of atom ...
... • Doppler shift– toward (blue) and away (red) • Quantum mechanics– electrons can be wave-like – Electrons around nucleus have certain orbits– defines emission and absorption of each atom – When excited, atoms emit certain lines (like in class)– fingerprint or barcode of atom ...
Learning Objectives - UNC Physics and Astronomy
... globular clusters to measure (1) our distance from the center of the Milky Way, and (2) the approximate size of the Milky Way. Shapely also argued that the Milky Way is so big that it is the primary object in the universe, and that what were then called “spiral nebulae”, like Andromeda, are nearby a ...
... globular clusters to measure (1) our distance from the center of the Milky Way, and (2) the approximate size of the Milky Way. Shapely also argued that the Milky Way is so big that it is the primary object in the universe, and that what were then called “spiral nebulae”, like Andromeda, are nearby a ...
Herschel Space Observatory - Science and Technology Facilities
... Cassiopeia A is all that remains of a massive star which exploded hundreds of years ago, in an event called a supernova. The explosion was not observed, most likely due to the thick clouds of dust which lie in between it and the Earth. Herschel sees the dust in our Galaxy, shown in red, as well as t ...
... Cassiopeia A is all that remains of a massive star which exploded hundreds of years ago, in an event called a supernova. The explosion was not observed, most likely due to the thick clouds of dust which lie in between it and the Earth. Herschel sees the dust in our Galaxy, shown in red, as well as t ...
Andromeda Nebula Lies Outside Milky Way Galaxy
... closer to Earth. As reported in a recent paper, Hubble's measurements led him to a useful speeddistance relationship: redshifts increase in direct proportion to their distance from us. Dr. Hubble determined distances to the twenty-four nebula using Cepheid variable stars. These are stars that astron ...
... closer to Earth. As reported in a recent paper, Hubble's measurements led him to a useful speeddistance relationship: redshifts increase in direct proportion to their distance from us. Dr. Hubble determined distances to the twenty-four nebula using Cepheid variable stars. These are stars that astron ...
The supernova of AD1181 – an update
... The Crab nebula and 3C 58 are both members of the “filled-centre” class of SNRs, which contains about 10 known objects in the Galaxy, all of which show such centrally brightened morphologies. (These SNRs are also called “Crab-like” remnants, although it is not clear whether or not the Crab is typica ...
... The Crab nebula and 3C 58 are both members of the “filled-centre” class of SNRs, which contains about 10 known objects in the Galaxy, all of which show such centrally brightened morphologies. (These SNRs are also called “Crab-like” remnants, although it is not clear whether or not the Crab is typica ...
Stars (Ch. 13)
... can determine its luminosity. • A stars luminosity is related to both its temperature and its radius. • So if we also know a star’s temperature we can determine its ...
... can determine its luminosity. • A stars luminosity is related to both its temperature and its radius. • So if we also know a star’s temperature we can determine its ...
August - Naples Free-Net
... Beginning in 1845, with the unveiling of Lord Rosse’s 6-foot (1.8 m) aperture telescope, several of the nebulae catalogued by Messier, Herschel and others were discovered to contain an internal spiral structure. The extreme light-gathering power afforded by this new telescope allowed us, for the fir ...
... Beginning in 1845, with the unveiling of Lord Rosse’s 6-foot (1.8 m) aperture telescope, several of the nebulae catalogued by Messier, Herschel and others were discovered to contain an internal spiral structure. The extreme light-gathering power afforded by this new telescope allowed us, for the fir ...
Death of the Stars
... The event horizon of black holes is too small to be optically observed from the Earth. Instead we must rely on indirect methods of observation. First, if a star seems to be rotating around “nothing”, that nothing is probably very small to be observed from the Earth, but very massive, hence it can be ...
... The event horizon of black holes is too small to be optically observed from the Earth. Instead we must rely on indirect methods of observation. First, if a star seems to be rotating around “nothing”, that nothing is probably very small to be observed from the Earth, but very massive, hence it can be ...
Star Formation in Disks: Spiral Arms, Turbulence, and Triggering
... other cloud, then M 2 dN/dM = constant again. This may be seen with a simple example. Imagine clouds subdivided by twos: one cloud of mass 32 units divided into 2 clouds of mass 16 units, which are each divided into 2 more clouds of 8 units, and so on until the smallest level, which has 32 clouds of ...
... other cloud, then M 2 dN/dM = constant again. This may be seen with a simple example. Imagine clouds subdivided by twos: one cloud of mass 32 units divided into 2 clouds of mass 16 units, which are each divided into 2 more clouds of 8 units, and so on until the smallest level, which has 32 clouds of ...
Starlight and Atoms - School District of Clayton
... Light and Matter Spectra of stars are more complicated than pure blackbody spectra. characteristic lines, called absorption lines. To understand those lines, we need to understand atomic structure and the interactions between light and atoms. ...
... Light and Matter Spectra of stars are more complicated than pure blackbody spectra. characteristic lines, called absorption lines. To understand those lines, we need to understand atomic structure and the interactions between light and atoms. ...
HR Diagram Explorer Worksheet
... Question 6: Use the results from the previous 5 questions to construct a “conceptual” HR Diagram. You simply want to draw arrows showing the direction in which variables are increasing. a) Draw in an arrow on the y axis showing the direction of increasing “intrinsic luminosity” of the stars. (This ...
... Question 6: Use the results from the previous 5 questions to construct a “conceptual” HR Diagram. You simply want to draw arrows showing the direction in which variables are increasing. a) Draw in an arrow on the y axis showing the direction of increasing “intrinsic luminosity” of the stars. (This ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... It is thrown off at a speed as high as 1/10 the speed of light. The hot exploding gas can emit as much light as 1010 Suns for a few days. (Even more energy comes out in the form of neutrinos, but they are very hard to detect.) This happened in the Large Magellanic Cloud (a group of about 108 stars a ...
... It is thrown off at a speed as high as 1/10 the speed of light. The hot exploding gas can emit as much light as 1010 Suns for a few days. (Even more energy comes out in the form of neutrinos, but they are very hard to detect.) This happened in the Large Magellanic Cloud (a group of about 108 stars a ...
Lesson Overviews and Content Standards
... galaxies students will move from the 1 to 10 billion scale model used with stars to one showing the size of the Milky Way in comparison to the spacing between galaxies in the Local Group. Images of our galactic neighbors are provided for the teacher to enrich the introduction to galaxies beyond our ...
... galaxies students will move from the 1 to 10 billion scale model used with stars to one showing the size of the Milky Way in comparison to the spacing between galaxies in the Local Group. Images of our galactic neighbors are provided for the teacher to enrich the introduction to galaxies beyond our ...
luminosities
... Example: Star Radii Polaris has just about the same spectral type (and thus surface temperature) as our sun, but it is 10,000 times brighter than our sun. ...
... Example: Star Radii Polaris has just about the same spectral type (and thus surface temperature) as our sun, but it is 10,000 times brighter than our sun. ...
The Solar Neighborhood
... What general trends do you see in the data in the plot? Draw a line following the main sequence defined by the nearest and the brightest stars together. Draw a circle encompassing any white dwarf stars and a circle encompassing any giant or supergiant stars. List the giants and supergiants below. Al ...
... What general trends do you see in the data in the plot? Draw a line following the main sequence defined by the nearest and the brightest stars together. Draw a circle encompassing any white dwarf stars and a circle encompassing any giant or supergiant stars. List the giants and supergiants below. Al ...
ph507lecnote06
... The emission lines can only occur if the gas in the chromosphere is very hot and the density is very low. The chromosphere is hotter (but less dense) than the photosphere. In the spicules, which are best observed in H , gas is rising at about 20 to 25 km/s. Although spicules occupy less than 1% of t ...
... The emission lines can only occur if the gas in the chromosphere is very hot and the density is very low. The chromosphere is hotter (but less dense) than the photosphere. In the spicules, which are best observed in H , gas is rising at about 20 to 25 km/s. Although spicules occupy less than 1% of t ...
Prof. Kenney C lass 8 September 26, 2016
... star during normal stellar evolution get locked into neutron star or black hole core ...
... star during normal stellar evolution get locked into neutron star or black hole core ...
Chapter 15 Surveying the Stars
... Amount of starlight that reaches Earth (energy per second per square meter) ...
... Amount of starlight that reaches Earth (energy per second per square meter) ...
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.