Integrated Science
... massive stars which have mass greater than 4 to 8 times that of our Sun. After these stars have finished burning their nuclear fuel, they undergo a supernova explosion. This explosion blows off the outer layers of a star into a beautiful supernova remnant. The central region of the star collapses ...
... massive stars which have mass greater than 4 to 8 times that of our Sun. After these stars have finished burning their nuclear fuel, they undergo a supernova explosion. This explosion blows off the outer layers of a star into a beautiful supernova remnant. The central region of the star collapses ...
key for the HR Diagram Lab Handout
... Geminorum have brightness of 9,000 Suns and 310 Suns respectively; these stars are much larger than Proxima and Barnard s with brightness of 0.00005 and 0.0003 Suns. The significant difference in brightness with no change in temperature means that Betelgeuse and Mu Geminorum are much larger than the ...
... Geminorum have brightness of 9,000 Suns and 310 Suns respectively; these stars are much larger than Proxima and Barnard s with brightness of 0.00005 and 0.0003 Suns. The significant difference in brightness with no change in temperature means that Betelgeuse and Mu Geminorum are much larger than the ...
The Life Cycle of Spiral Arm Galaxies
... As a star goes supernova, it releases a great amount of energy (light) and also ejects a massive amount of matter (galactic cosmic rays), which are charged particles such as protons and pieces of ...
... As a star goes supernova, it releases a great amount of energy (light) and also ejects a massive amount of matter (galactic cosmic rays), which are charged particles such as protons and pieces of ...
CCD BVRI and 2MASS Photometry of the Poorly Studied Open
... NGC 6631. It is observed from the 1.88 m Telescope of Kottamia Observatory in Egypt. About 3300 stars have been observed in an area of ∼ 10′ × 10′ around the cluster center. The main photometric parameters have been estimated and compared with the results that determined for the cluster using JHKs 2 ...
... NGC 6631. It is observed from the 1.88 m Telescope of Kottamia Observatory in Egypt. About 3300 stars have been observed in an area of ∼ 10′ × 10′ around the cluster center. The main photometric parameters have been estimated and compared with the results that determined for the cluster using JHKs 2 ...
slides - Indico
... for Galactic Chemical Evolution Timothy C. Beers Department of Physics & Astronomy and JINA: Joint Institute for Nuclear Astrophysics Michigan State University ...
... for Galactic Chemical Evolution Timothy C. Beers Department of Physics & Astronomy and JINA: Joint Institute for Nuclear Astrophysics Michigan State University ...
The Formation of Stars and Solar Systems
... is found in normal interstellar space, many atoms combine into molecules molecular hydrogen (H2), and the gas cloud becomes a molecular cloud. • A molecular cloud is sometimes called a stellar nursery if star formation is occurring within it. • Like clouds in our sky, these molecular clouds are puff ...
... is found in normal interstellar space, many atoms combine into molecules molecular hydrogen (H2), and the gas cloud becomes a molecular cloud. • A molecular cloud is sometimes called a stellar nursery if star formation is occurring within it. • Like clouds in our sky, these molecular clouds are puff ...
ASTRONOMY AND ASTROPHYSICS Letter to the Editor Low
... masses. Because of ≈ 10 magnitudes range in luminosities in the crowded core region our sensitivity limits of Js ≈ 21m , H ≈ 20m and Ks ≈ 19m don’t appear to be exceedingly faint (and are about 3 magnitudes above ISAAC’s detection limit for isolated sources). However, only VLT/ISAAC’s high angular r ...
... masses. Because of ≈ 10 magnitudes range in luminosities in the crowded core region our sensitivity limits of Js ≈ 21m , H ≈ 20m and Ks ≈ 19m don’t appear to be exceedingly faint (and are about 3 magnitudes above ISAAC’s detection limit for isolated sources). However, only VLT/ISAAC’s high angular r ...
Compa ring between Spectroscopic and Photometric Method for
... are visible, sequence of observations would indicate that the stars move around a common center of gravity. Observations indicate that majority of stars have a companion, thus that stars are in more than 50% of cases united in a system of two or more stars. Multiple systems consist of stars, which a ...
... are visible, sequence of observations would indicate that the stars move around a common center of gravity. Observations indicate that majority of stars have a companion, thus that stars are in more than 50% of cases united in a system of two or more stars. Multiple systems consist of stars, which a ...
HOU Supernova Light Curves
... In the spring of 1994 several HOU students were studying M51, the spiral galaxy also known as the Whirlpool Galaxy. Various HOU images had been requested throughout February and March, and in early April, two girls at Oil City High School in Pennsylvania received an important phone call. They had se ...
... In the spring of 1994 several HOU students were studying M51, the spiral galaxy also known as the Whirlpool Galaxy. Various HOU images had been requested throughout February and March, and in early April, two girls at Oil City High School in Pennsylvania received an important phone call. They had se ...
01-Star Atlas Project - Mapping the Heavens
... Apparent means what it says, how does it "appear " from where you're standing. If you're standing upon the Earth, it will appear quite differently than if you're standing on ...
... Apparent means what it says, how does it "appear " from where you're standing. If you're standing upon the Earth, it will appear quite differently than if you're standing on ...
Galactic Star Formation Science with Integral Field
... – 170+ Emission lines detected – Many very high excitation lines of H2 and [Fe II] – Bow-shock apex shows extremely high temperature T~6000K - revealing that the H2 molecule persists in these very high temperature regions Giannini et al. “Near-infrared, IFU spectroscopy unravels the bow-shock HH99B“ ...
... – 170+ Emission lines detected – Many very high excitation lines of H2 and [Fe II] – Bow-shock apex shows extremely high temperature T~6000K - revealing that the H2 molecule persists in these very high temperature regions Giannini et al. “Near-infrared, IFU spectroscopy unravels the bow-shock HH99B“ ...
Barium Stars Observed with the Coude Echelle Spectrometer
... the postulated resonant coupling is much more likely in rapidly rotating stars. This is a nice result since Be stars are the lastest rotators on the right of the zero-age main sequence in the H-R diagram. Simulations with the above-mentioned computer programme demonstrate that (not surprisingly) the ...
... the postulated resonant coupling is much more likely in rapidly rotating stars. This is a nice result since Be stars are the lastest rotators on the right of the zero-age main sequence in the H-R diagram. Simulations with the above-mentioned computer programme demonstrate that (not surprisingly) the ...
presentation source
... “[Even though T Tauri associations could all have similar colors implying young age by coincidence], it is of course, tempting to search for a connection between the T Tauri stars and Bok’s ‘globules,’ but we must admit that at present there is no evidence of any objects intermediate between the two ...
... “[Even though T Tauri associations could all have similar colors implying young age by coincidence], it is of course, tempting to search for a connection between the T Tauri stars and Bok’s ‘globules,’ but we must admit that at present there is no evidence of any objects intermediate between the two ...
10 New Constellations
... Also known as Alpha Persei, Mirfak is located around 500 light years from Earth and is the brightest star in the constellation, it's a white supergiant with a diameter around 30 times larger than the sun. Algol Also known as Beta Persei, Algol is actually a three star system located around 90 light ...
... Also known as Alpha Persei, Mirfak is located around 500 light years from Earth and is the brightest star in the constellation, it's a white supergiant with a diameter around 30 times larger than the sun. Algol Also known as Beta Persei, Algol is actually a three star system located around 90 light ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.