LOW MASS STAR FORMATION
... SO (55 – 44) traces hot ( > 40 K) and dense (~ 106 cm-3) gas (Chernin et al. 1994). From SO spectrum a column density of N(SO)= 2.5 – 3.4 x 1014 cm-2 is derived for temperatures of 50 – 100 K. Assuming [SO/H2 ] of 0.5 – 2.0 x 10-8 (Helmich & Dishoeck 1997) a mass of 0.7 – 3.5 Msol is derived. ...
... SO (55 – 44) traces hot ( > 40 K) and dense (~ 106 cm-3) gas (Chernin et al. 1994). From SO spectrum a column density of N(SO)= 2.5 – 3.4 x 1014 cm-2 is derived for temperatures of 50 – 100 K. Assuming [SO/H2 ] of 0.5 – 2.0 x 10-8 (Helmich & Dishoeck 1997) a mass of 0.7 – 3.5 Msol is derived. ...
Document
... ~60 hard sources down to 1035 erg/s within 1kpc of the Galactic center, 2000 sources down to 1031 erg/s within ~20kpc, If Portegies Zwart’s team’s estimates are correct, then several hundred of these hard, weak X-ray sources (10–20% of them) could be IMBHs. This fraction would not contradict current ...
... ~60 hard sources down to 1035 erg/s within 1kpc of the Galactic center, 2000 sources down to 1031 erg/s within ~20kpc, If Portegies Zwart’s team’s estimates are correct, then several hundred of these hard, weak X-ray sources (10–20% of them) could be IMBHs. This fraction would not contradict current ...
SIERRA STAR GAZERS
... drifting upward from the spout. We’ll observe some of the magnificent objects in the vicinity of the teapot, then pick up the remaining jewels next moth. Messier 22 is an outstanding 5th magnitude globular cluster. Over 500,000 stars make up this teeming conglomeration of lights that extends across ...
... drifting upward from the spout. We’ll observe some of the magnificent objects in the vicinity of the teapot, then pick up the remaining jewels next moth. Messier 22 is an outstanding 5th magnitude globular cluster. Over 500,000 stars make up this teeming conglomeration of lights that extends across ...
Orbital Instabilities in Triaxial Mass Distributions and
... with b < 225 AU to avoid disruption of Neptune, etc. [4] Solar system must live in its birth cluster for a relatively long time (100 Myr), a 10 percent effect. [5] Oort Cloud would be stripped in the birth cluster, so it must form after solar system leaves. [6] Orbits can be damped (in principle) af ...
... with b < 225 AU to avoid disruption of Neptune, etc. [4] Solar system must live in its birth cluster for a relatively long time (100 Myr), a 10 percent effect. [5] Oort Cloud would be stripped in the birth cluster, so it must form after solar system leaves. [6] Orbits can be damped (in principle) af ...
Lecture 7
... are quite red---their star-forming phase is nearly over, and their average stars are quite old. Sd’s in contrast have a lot of gas and have a long life of star forming ahead. They look clumpy because their light is dominated by young stars, which form in clumps of interstellar gas. (These stellar cl ...
... are quite red---their star-forming phase is nearly over, and their average stars are quite old. Sd’s in contrast have a lot of gas and have a long life of star forming ahead. They look clumpy because their light is dominated by young stars, which form in clumps of interstellar gas. (These stellar cl ...
Sample Midterm - IUPUI Physics
... 14. Why would using a cluster of stars in which all the stars are the same distance to plot on an HR diagram be very useful? a) The stars would then all be the same brightness b) The stars would then all be the same color c) Stars with different apparent magnitudes have different absolute magnitudes ...
... 14. Why would using a cluster of stars in which all the stars are the same distance to plot on an HR diagram be very useful? a) The stars would then all be the same brightness b) The stars would then all be the same color c) Stars with different apparent magnitudes have different absolute magnitudes ...
GEARS Workshop Monday - Georgia Southern University
... • Let’s think back to initial categories made of star image • Having made a few measurements now – let’s list the intrinsic properties of stars on the board together ...
... • Let’s think back to initial categories made of star image • Having made a few measurements now – let’s list the intrinsic properties of stars on the board together ...
Week8Lecture1
... Our Galaxy is a spiral galaxy. Here are two other spiral galaxies, one viewed from the side and the other from the top, which are thought to resemble the Milky Way: ...
... Our Galaxy is a spiral galaxy. Here are two other spiral galaxies, one viewed from the side and the other from the top, which are thought to resemble the Milky Way: ...
CONSTELLATION TUCANA, THE TOUCAN
... arcminutes away from the bigger cluster's edge, and Lindsay 8. NGC 362 is another globular cluster in Tucana with an apparent magnitude of 6.4, 27,700 light-years from Earth. Like neighboring 47 Tucanae, NGC 362 is a Shapley class III cluster and among the brightest globular clusters in the sky. Unu ...
... arcminutes away from the bigger cluster's edge, and Lindsay 8. NGC 362 is another globular cluster in Tucana with an apparent magnitude of 6.4, 27,700 light-years from Earth. Like neighboring 47 Tucanae, NGC 362 is a Shapley class III cluster and among the brightest globular clusters in the sky. Unu ...
Life on the Main Sequence + Expansion to Red Giant
... Mmax ~ 100 solar masses a) More massive clouds fragment into smaller pieces during star formation. ...
... Mmax ~ 100 solar masses a) More massive clouds fragment into smaller pieces during star formation. ...
Examining the M67 Classification as an Open Cluster
... the cluster. It turned out that the characteristic time for this process of destruction of dense stellar clusters is at most 1010 yr. Spitzer [16,17] has calculated the increase of energy leading to desintegration of a cluster due to encounters with interstellar clouds. Spitzer has argued that the c ...
... the cluster. It turned out that the characteristic time for this process of destruction of dense stellar clusters is at most 1010 yr. Spitzer [16,17] has calculated the increase of energy leading to desintegration of a cluster due to encounters with interstellar clouds. Spitzer has argued that the c ...
Stars
... low density outer envelope completely off the star. • As it expands, its opacity drops and we see to a deeper and deeper and hotter and hotter depth, so the star moves left on the HR diagram • Until… we see the electron degenerate core; the new white dwarf created at the center • This core can now c ...
... low density outer envelope completely off the star. • As it expands, its opacity drops and we see to a deeper and deeper and hotter and hotter depth, so the star moves left on the HR diagram • Until… we see the electron degenerate core; the new white dwarf created at the center • This core can now c ...
PH607lec12
... This cluster is loaded with gas and dust rich, star forming, spiral galaxies but has relatively few elliptical galaxies, which lack gas and dust and the associated newborn stars. Colours in the composite image show the star forming galaxies with a blue tint and ellipticals with a slightly yellowish ...
... This cluster is loaded with gas and dust rich, star forming, spiral galaxies but has relatively few elliptical galaxies, which lack gas and dust and the associated newborn stars. Colours in the composite image show the star forming galaxies with a blue tint and ellipticals with a slightly yellowish ...
Star formation jeopardy
... only known star to support a planet with life. Why is our star (the sun) frequently referred to as an “average” star? Compare the important physical characteristics of the Sun with the most common types of stars. ...
... only known star to support a planet with life. Why is our star (the sun) frequently referred to as an “average” star? Compare the important physical characteristics of the Sun with the most common types of stars. ...
PHYS 2410 General Astronomy Homework 8
... as the material slows down it converts thermal energy to gravitational potential energy. ...
... as the material slows down it converts thermal energy to gravitational potential energy. ...
6th Grade Science Chapter 19 Jeopardy Game
... a. New stars form from the material of old stars. b. A star does not change its’ size or temperature during its’ life. c. The shortest stage in a star’s life cycle is the main sequence. ...
... a. New stars form from the material of old stars. b. A star does not change its’ size or temperature during its’ life. c. The shortest stage in a star’s life cycle is the main sequence. ...
Nebulae
... Trigger of Star Birth: Shock Waves from O and B Stars • The most massive protostars to form out of a dark nebula rapidly become main sequence O and B stars • They emit strong ultraviolet radiation that ionizes hydrogen in the surrounding cloud, thus creating the reddish emission nebulae called H II ...
... Trigger of Star Birth: Shock Waves from O and B Stars • The most massive protostars to form out of a dark nebula rapidly become main sequence O and B stars • They emit strong ultraviolet radiation that ionizes hydrogen in the surrounding cloud, thus creating the reddish emission nebulae called H II ...
![Gugus Bintang [Compatibility Mode]](http://s1.studyres.com/store/data/007745973_1-cdf92b37339f4354c66eef546bd46492-300x300.png)
The Galaxy Presentation 2011
... Rotation Curve of MWG - v is almost constant or slightly increasing with distance from center! ...
... Rotation Curve of MWG - v is almost constant or slightly increasing with distance from center! ...
globular cluster - Harding University
... Determine our Place in the Milky Way Shapley made use of RR Lyra variable stars found in many globular clusters to determine the distances to these clusters. RR Lyra variables, like the Cepheid variables also have a period – luminosity relationship. By measuring the distances to, and the relativ ...
... Determine our Place in the Milky Way Shapley made use of RR Lyra variable stars found in many globular clusters to determine the distances to these clusters. RR Lyra variables, like the Cepheid variables also have a period – luminosity relationship. By measuring the distances to, and the relativ ...
Last Year`s Exam, Section B
... iron fusion does not generate energy when iron core gets too big, it will collapse, and cannot be saved by fusion iron core collapses to neutron star (or, for star as massive as θ1 Orionis C, perhaps black hole) infalling outer regions bounce off rigid neutron star ...
... iron fusion does not generate energy when iron core gets too big, it will collapse, and cannot be saved by fusion iron core collapses to neutron star (or, for star as massive as θ1 Orionis C, perhaps black hole) infalling outer regions bounce off rigid neutron star ...
Two Summers in the UCSC Science Internship Program
... Science that year, I hoped to apply computer programming to cutting-edge research in astrophysics. I was excited when I was assigned to work with Dr. Guhathakurta and Dr. Evan Kirby of Caltech, as well as another high school student who was my partner. ...
... Science that year, I hoped to apply computer programming to cutting-edge research in astrophysics. I was excited when I was assigned to work with Dr. Guhathakurta and Dr. Evan Kirby of Caltech, as well as another high school student who was my partner. ...
Open cluster
An open cluster, also known as galactic cluster, is a group of up to a few thousand stars that were formed from the same giant molecular cloud and have roughly the same age. More than 1,100 open clusters have been discovered within the Milky Way Galaxy, and many more are thought to exist. They are loosely bound by mutual gravitational attraction and become disrupted by close encounters with other clusters and clouds of gas as they orbit the galactic center, resulting in a migration to the main body of the galaxy as well as a loss of cluster members through internal close encounters. Open clusters generally survive for a few hundred million years, with the most massive ones surviving for a few billion years. In contrast, the more massive globular clusters of stars exert a stronger gravitational attraction on their members, and can survive for longer. Open clusters have been found only in spiral and irregular galaxies, in which active star formation is occurring.Young open clusters may still be contained within the molecular cloud from which they formed, illuminating it to create an H II region. Over time, radiation pressure from the cluster will disperse the molecular cloud. Typically, about 10% of the mass of a gas cloud will coalesce into stars before radiation pressure drives the rest of the gas away.Open clusters are key objects in the study of stellar evolution. Because the cluster members are of similar age and chemical composition, their properties (such as distance, age, metallicity and extinction) are more easily determined than they are for isolated stars. A number of open clusters, such as the Pleiades, Hyades or the Alpha Persei Cluster are visible with the naked eye. Some others, such as the Double Cluster, are barely perceptible without instruments, while many more can be seen using binoculars or telescopes. The Wild Duck Cluster, M11, is an example.