TAURUS ZODIAC CONSTELLATION In Greek mythology, Taurus
... Athena. Taurus marks the end of an area in the sky that the ancients referred to as the sea - the region from Capricorn to the region containing Aries. It was referred to as the sea due to the high concentration of constellations identified as sea creatures within it; Aries included because of being ...
... Athena. Taurus marks the end of an area in the sky that the ancients referred to as the sea - the region from Capricorn to the region containing Aries. It was referred to as the sea due to the high concentration of constellations identified as sea creatures within it; Aries included because of being ...
Topics for Today`s Class Luminosity Equation The Heart of
... • In an H–R diagram, a star is represented by a dot at a position that shows the star’s luminosity and temperature. • The background color in this diagram indicates the temperature of the stars. • The Sun is a yellow-white G2 star. • Most stars including the Sun have properties along the mainsequenc ...
... • In an H–R diagram, a star is represented by a dot at a position that shows the star’s luminosity and temperature. • The background color in this diagram indicates the temperature of the stars. • The Sun is a yellow-white G2 star. • Most stars including the Sun have properties along the mainsequenc ...
Deep Space Mystery Note Form 3
... Small core of neutrons Spinning neutron star. Neutrons produce radio waves in a steady stream or random bursts. Stars 10 times the sun will leave a black hole. Leave behind a large core. With no energy fuse, it doesn’t have any out ward pressure so it gets engulfed in it’s own gravity an ...
... Small core of neutrons Spinning neutron star. Neutrons produce radio waves in a steady stream or random bursts. Stars 10 times the sun will leave a black hole. Leave behind a large core. With no energy fuse, it doesn’t have any out ward pressure so it gets engulfed in it’s own gravity an ...
The Hertzsprung-Russell Diagram
... Equal Radius Lines In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
... Equal Radius Lines In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
Binary Orbits
... determine parameters e.g. period and line of sight velocities – masses – done in optical and X-ray • Fact that a large fraction of stars are found in binaries indicate stars are formed in groups through gravitational collapse of ...
... determine parameters e.g. period and line of sight velocities – masses – done in optical and X-ray • Fact that a large fraction of stars are found in binaries indicate stars are formed in groups through gravitational collapse of ...
here - SDSU Astronomy Department and Mount Laguna Observatory
... • From the star counts, it was concluded that the “Universe” is a flattened structure (aspect ratio of 5:1) with a diameter of about 8000 light years. The Sun was essentially at the center. • Either we are at a very special place, or something is wrong. Interstellar dust was not accounted for. ...
... • From the star counts, it was concluded that the “Universe” is a flattened structure (aspect ratio of 5:1) with a diameter of about 8000 light years. The Sun was essentially at the center. • Either we are at a very special place, or something is wrong. Interstellar dust was not accounted for. ...
The H-R Diagram
... The Random Walk towards the Spectral Types… • White Stars, with prominent hydrogen lines. Called them “A stars.” • Blue-white stars, with less prominent H lines, and weak helium lines. Called them “B stars” • Then, no more in this color direction, so skip some letters and… Cream colored stars, with ...
... The Random Walk towards the Spectral Types… • White Stars, with prominent hydrogen lines. Called them “A stars.” • Blue-white stars, with less prominent H lines, and weak helium lines. Called them “B stars” • Then, no more in this color direction, so skip some letters and… Cream colored stars, with ...
LANL Cosmology Summer School Lectures, July 2010
... ULIRGs: X = 0.8 MO/(K km/s pc^2) (CO rotation curves) Optically thin limit: X ~ 0.2 ...
... ULIRGs: X = 0.8 MO/(K km/s pc^2) (CO rotation curves) Optically thin limit: X ~ 0.2 ...
slides - Indico
... first generations of stars in the Universe • The shape of the low-metallicity tail of the Metallicity Distribution Function will (eventually) show structure that reveals the characteristic abundances of major epochs of star formation in early Galaxy • Identification of relatively rare objects amongs ...
... first generations of stars in the Universe • The shape of the low-metallicity tail of the Metallicity Distribution Function will (eventually) show structure that reveals the characteristic abundances of major epochs of star formation in early Galaxy • Identification of relatively rare objects amongs ...
A new isolated dSph galaxy near the Local Group
... & Tully (2009) in the nearby group around M81. The discoveries resulted from targeted searches within small parts of the sky (∼390 and ∼65 deg2 , respectively). The hunt for isolated spheroidal dwarfs is very difficult because it requires a survey of large sky area and considerable sensitivity. Obje ...
... & Tully (2009) in the nearby group around M81. The discoveries resulted from targeted searches within small parts of the sky (∼390 and ∼65 deg2 , respectively). The hunt for isolated spheroidal dwarfs is very difficult because it requires a survey of large sky area and considerable sensitivity. Obje ...
DTU_9e_ch13
... from one of the first pulsars to be discovered, PSR 0329 + 54. Note that some of the pulses are weak and others are strong. Nevertheless, the spacing between pulses is so regular (0.714 s) that it is more precise than most clocks on Earth. ...
... from one of the first pulsars to be discovered, PSR 0329 + 54. Note that some of the pulses are weak and others are strong. Nevertheless, the spacing between pulses is so regular (0.714 s) that it is more precise than most clocks on Earth. ...
Chapter 1 Section Misconception Truth Distances in the Universe
... The Photosphere The Sun and stars have absorption spectra because the photosphere is cooler than the core. All the light we see comes from the photosphere; the core is well hidden below hundreds of thousands of kilometers of solar gas. The absorption lines and the continuum are both formed in the ...
... The Photosphere The Sun and stars have absorption spectra because the photosphere is cooler than the core. All the light we see comes from the photosphere; the core is well hidden below hundreds of thousands of kilometers of solar gas. The absorption lines and the continuum are both formed in the ...
Stars
... •With Newton’s modifications to Kepler’s laws, the period and size of the orbits yield the sum of the masses, while the relative distance of each star from the center of mass yields the ratio of the masses. •The ratio and sum provide each mass individually. ...
... •With Newton’s modifications to Kepler’s laws, the period and size of the orbits yield the sum of the masses, while the relative distance of each star from the center of mass yields the ratio of the masses. •The ratio and sum provide each mass individually. ...
superbubbles vs super-galactic winds
... the densest regions of the host galaxies. However, supergalactic winds are able to channel the metals produced by the recent burst straight into the intergalactic medium while superbubbles fail to reach the outskirts of the host galaxies and thus retain the newly processed metals and with them event ...
... the densest regions of the host galaxies. However, supergalactic winds are able to channel the metals produced by the recent burst straight into the intergalactic medium while superbubbles fail to reach the outskirts of the host galaxies and thus retain the newly processed metals and with them event ...
Announcements - Lick Observatory
... Galaxy, but for the vast majority, the separation of the stars is large enough that one star doesn’t affect the evolution of the other(s). ...
... Galaxy, but for the vast majority, the separation of the stars is large enough that one star doesn’t affect the evolution of the other(s). ...
White dwarfs & supernovae — Oct 19 white dwarfs?
... 1. Plot shows the speed of a normal gas made of electrons with a temperature of 1000K and a degenerate gas of electrons with a temperature of 0K. A. I is a NG. II is a DG. B. I is a DG. II is a NG. ...
... 1. Plot shows the speed of a normal gas made of electrons with a temperature of 1000K and a degenerate gas of electrons with a temperature of 0K. A. I is a NG. II is a DG. B. I is a DG. II is a NG. ...
Galaxies and Their Structure
... •This is a 2048x2048 CCD image of the Coma Cluster. This cluster has a recessional velocity of about 7000 km/s and is the densest cluster in our local region of the Universe. In contrast to the Hercules cluster, Coma has almost no spiral galaxies in its central regions. The cluster is strongly viri ...
... •This is a 2048x2048 CCD image of the Coma Cluster. This cluster has a recessional velocity of about 7000 km/s and is the densest cluster in our local region of the Universe. In contrast to the Hercules cluster, Coma has almost no spiral galaxies in its central regions. The cluster is strongly viri ...
Indroduction
... more recent ones by Kau mann & Charlot (1996), and Kau mann & Charlot (1997) ellipticals are viewed as being formed by mergers of disk galaxies in a universe where structures are built through hierarchical clustering. In the local universe, ongoing merging is observed and it is generally assumed tha ...
... more recent ones by Kau mann & Charlot (1996), and Kau mann & Charlot (1997) ellipticals are viewed as being formed by mergers of disk galaxies in a universe where structures are built through hierarchical clustering. In the local universe, ongoing merging is observed and it is generally assumed tha ...
![31 — Main-Sequence Stars [Revision : 1.1]](http://s1.studyres.com/store/data/015926256_1-97d746cbe97ccc13b433136b208bf071-300x300.png)
31 — Main-Sequence Stars [Revision : 1.1]
... – Difference due to differing abundance/molecular weight distribution in cores ∗ Low-mass stars have smoothly varying abundance change ∗ High-mass stars have discontinuous abundance chage (although discontinuity smeared out by core shrinkage), due to convective mixing ∗ Very-low-mass stars (. 0.3 M ...
... – Difference due to differing abundance/molecular weight distribution in cores ∗ Low-mass stars have smoothly varying abundance change ∗ High-mass stars have discontinuous abundance chage (although discontinuity smeared out by core shrinkage), due to convective mixing ∗ Very-low-mass stars (. 0.3 M ...
Investigate Stars and Galaxies - American Museum of Natural History
... Using the information in the diagram and also in the sections on star type you used in the chart in Step 2, record the following information about each star: (Teacher’s Note: Because the HR diagram only designates some temperatures ...
... Using the information in the diagram and also in the sections on star type you used in the chart in Step 2, record the following information about each star: (Teacher’s Note: Because the HR diagram only designates some temperatures ...
closed-box model
... the Universe, while all metals (except for a very small fraction of Li) were produced through nucleosynthesis (nuclear burning) in stars. ...
... the Universe, while all metals (except for a very small fraction of Li) were produced through nucleosynthesis (nuclear burning) in stars. ...
Slide 1
... Star forming regions and interstellar medium physics in Milky Way and external galaxies Molecular chemistry of cometary, planetary and satellite atmospheres in solar system ...
... Star forming regions and interstellar medium physics in Milky Way and external galaxies Molecular chemistry of cometary, planetary and satellite atmospheres in solar system ...
G485 5.5.1 Structure of the Universe
... having a mean diameter of about 100 000 light-years (ly). The Sun, one of the billions of stars in the Milky Way, is located at a point about 28 000 ly from the galactic centre and it takes about 230 million years to complete one revolution. ...
... having a mean diameter of about 100 000 light-years (ly). The Sun, one of the billions of stars in the Milky Way, is located at a point about 28 000 ly from the galactic centre and it takes about 230 million years to complete one revolution. ...
AyC10 Fall 2007: Midterm 2 Review Sheet
... parallax or other methods we haven’t discussed in detail). Once we know those two quantities, we use the equation b = L / 4d2 to compute the luminosity. CS 160-168 What does it mean for a star to be on the Main Sequence? A star is on the Main Sequence when its core is fusing hydrogen into helium. D ...
... parallax or other methods we haven’t discussed in detail). Once we know those two quantities, we use the equation b = L / 4d2 to compute the luminosity. CS 160-168 What does it mean for a star to be on the Main Sequence? A star is on the Main Sequence when its core is fusing hydrogen into helium. D ...
ASTR 340 - TerpConnect
... Figure 2.11: Virgo an irregular cluster is the nearest large cluster of galaxies (103-104 ...
... Figure 2.11: Virgo an irregular cluster is the nearest large cluster of galaxies (103-104 ...
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.