GEARS Workshop Monday - Georgia Southern University
... • More massive stars – short lived • Low mass stars – long lived • Range – 100,000 years – 100 billion years! ...
... • More massive stars – short lived • Low mass stars – long lived • Range – 100,000 years – 100 billion years! ...
RTFS Test - 2017 BCS Cobra
... What is the name of this “critical mass”? 72. What type of supernova results from a white dwarf gaining too much mass and exploding? 73. What will a cloud fragment with a mass of 0.02 times the mass of the Sun will evolve into? 74. How can we determine the mass of a star? 75. Two stars are each obse ...
... What is the name of this “critical mass”? 72. What type of supernova results from a white dwarf gaining too much mass and exploding? 73. What will a cloud fragment with a mass of 0.02 times the mass of the Sun will evolve into? 74. How can we determine the mass of a star? 75. Two stars are each obse ...
Chapter 11
... In the Orion Nebula The BecklinNeugebauer Object (BN): Hot star, just reaching the main sequence ...
... In the Orion Nebula The BecklinNeugebauer Object (BN): Hot star, just reaching the main sequence ...
homework assignment 2
... Some Misconceptions About Stars and Galaxies Misconception #1: The dimmer the star, the smaller it is. Misconception #2: You can tell how big (diameter) a star is by looking at it through a telescope. Misconception #3: All stars that you can see at night are white. Misconception #4: All stars in a ...
... Some Misconceptions About Stars and Galaxies Misconception #1: The dimmer the star, the smaller it is. Misconception #2: You can tell how big (diameter) a star is by looking at it through a telescope. Misconception #3: All stars that you can see at night are white. Misconception #4: All stars in a ...
What is Epsilon Aurigae?
... • Very massive?, could it form planets? • Low mass? , could it form planets? •Is there a central object(s)? • Disk Morphology? Disk, “donut”, ring, gaps? Thick, thin? etc.. ...
... • Very massive?, could it form planets? • Low mass? , could it form planets? •Is there a central object(s)? • Disk Morphology? Disk, “donut”, ring, gaps? Thick, thin? etc.. ...
matthewchristianstarprodject
... hydrogen atoms into helium. During this stage of the star's lifetime, it is determined by its mass, but also based upon its chemical composition and other factors. All main sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the core is balanced by the inward gravita ...
... hydrogen atoms into helium. During this stage of the star's lifetime, it is determined by its mass, but also based upon its chemical composition and other factors. All main sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the core is balanced by the inward gravita ...
Circumpolar constellations
... constellations over an hour, but you will notice their positions change over three or four hours in one night. And you will certainly notice their changing positions over a month. ...
... constellations over an hour, but you will notice their positions change over three or four hours in one night. And you will certainly notice their changing positions over a month. ...
CloudsToSolarSystems_EXES
... Molecular gas (as mapped by CO emission) extends over even more of the space mapped out in previous image. ...
... Molecular gas (as mapped by CO emission) extends over even more of the space mapped out in previous image. ...
Astronomy and Survey of Information
... Doppler shift of the emitted light. • These systems are known as spectroscopic binaries. ...
... Doppler shift of the emitted light. • These systems are known as spectroscopic binaries. ...
EvoluGon of high mass stars Solar-‐type stars end their lives by
... to the forma=on of a rapidly rota=ng neutron star because of conserva=on of angular momentum (if the Sun was compressed into a radius of 10 km it would rotate at 1000 =mes per second). ...
... to the forma=on of a rapidly rota=ng neutron star because of conserva=on of angular momentum (if the Sun was compressed into a radius of 10 km it would rotate at 1000 =mes per second). ...
How Big Is Our Universe? - Harvard
... galaxies not as they are today, but as they looked long before there was life on Earth. Some galaxies are so far away that they appear as tiny smudges, even through the largest telescopes. It’s tough to determine how large or bright these fuzzy distant galaxies are. But astronomers can figure out th ...
... galaxies not as they are today, but as they looked long before there was life on Earth. Some galaxies are so far away that they appear as tiny smudges, even through the largest telescopes. It’s tough to determine how large or bright these fuzzy distant galaxies are. But astronomers can figure out th ...
Chapter 13 section 3
... different stages in the life of a star are shown in the illustration on this page and the next page. When hydrogen in the core of the star runs out, the core contracts and temperatures inside the star increase. The outer layers of the star expand and cool. In this late stage in its life cycle, a sta ...
... different stages in the life of a star are shown in the illustration on this page and the next page. When hydrogen in the core of the star runs out, the core contracts and temperatures inside the star increase. The outer layers of the star expand and cool. In this late stage in its life cycle, a sta ...
Lecture Eight (Powerpoint format) - Flash
... three years on the Hubble Space Telescope. The image covers roughly 1000 AU. The outflow appears to be highly sporadic, but it remains unclear how it is being powered or even which binary member is powering it. ...
... three years on the Hubble Space Telescope. The image covers roughly 1000 AU. The outflow appears to be highly sporadic, but it remains unclear how it is being powered or even which binary member is powering it. ...
The Death of High Mass Stars
... Chandrasekhar limit (1.44M) and the core cannot be supported by electron degeneracy pressure - core continues to collapse very quickly – less than 1/10 second! The 56Fe atoms use any energy produced in the collapse, so the core does not heat up. Iron atoms get destroyed in the ever collapsing core ...
... Chandrasekhar limit (1.44M) and the core cannot be supported by electron degeneracy pressure - core continues to collapse very quickly – less than 1/10 second! The 56Fe atoms use any energy produced in the collapse, so the core does not heat up. Iron atoms get destroyed in the ever collapsing core ...
Observations and Theoretical Models of Subdwarfs
... bugles of spirals, and globular clusters -- in other words, any region consisting solely of old stellar populations –and found that there was an inexplicable excess of ultraviolet radiation being emitting from the regions which could not be attributed to the observed stars [19]. This was later terme ...
... bugles of spirals, and globular clusters -- in other words, any region consisting solely of old stellar populations –and found that there was an inexplicable excess of ultraviolet radiation being emitting from the regions which could not be attributed to the observed stars [19]. This was later terme ...
![Gugus Bintang [Compatibility Mode]](http://s1.studyres.com/store/data/007745973_1-cdf92b37339f4354c66eef546bd46492-300x300.png)
Gugus Bintang [Compatibility Mode]
... 2. Identify stellar types (such as blue giant stars and red giant stars), determine luminosity from the type, measure brightness, and then calculate distance. If the giant star is in a cluster, then we can determine the distance to the cluster by using several giant stars in the cluster to get its d ...
... 2. Identify stellar types (such as blue giant stars and red giant stars), determine luminosity from the type, measure brightness, and then calculate distance. If the giant star is in a cluster, then we can determine the distance to the cluster by using several giant stars in the cluster to get its d ...
Properties of Supernovae
... Supernova explosions are the most powerful events in the Universe. In less than a second, about 1044 Joules of energy are released---about the same as the Sun has released in its entire lifetime! The explosion results from the death of a massive star which has consumed its entire fuel supply. The ap ...
... Supernova explosions are the most powerful events in the Universe. In less than a second, about 1044 Joules of energy are released---about the same as the Sun has released in its entire lifetime! The explosion results from the death of a massive star which has consumed its entire fuel supply. The ap ...
Evolved Stellar Populations
... kinematics of both the stars and gas. The best laboratories for these studies are galaxies of the Local Group and in particular the Magellanic Clouds (nearby, known distance, low extinction, …interacting irregular galaxies). Distinguish between cluster and field stars. A global picture of any ...
... kinematics of both the stars and gas. The best laboratories for these studies are galaxies of the Local Group and in particular the Magellanic Clouds (nearby, known distance, low extinction, …interacting irregular galaxies). Distinguish between cluster and field stars. A global picture of any ...
Death of Stars notes
... The Big Picture • When massive stars end their lives in titanic explosions called supernovae, the chemical elements forged in the stars’ interiors-and created in the heat and pressure of the explosion--are released into space as a debris cloud of hot gas and dust. • Scientists had evidence of such ...
... The Big Picture • When massive stars end their lives in titanic explosions called supernovae, the chemical elements forged in the stars’ interiors-and created in the heat and pressure of the explosion--are released into space as a debris cloud of hot gas and dust. • Scientists had evidence of such ...
Stars I - Astronomy Centre
... in the Sun, yet Jupiter, with 1/1000 of Sun’s mass, possesses more angular momentum than any other body including the Sun. Why? ...
... in the Sun, yet Jupiter, with 1/1000 of Sun’s mass, possesses more angular momentum than any other body including the Sun. Why? ...
Cosmic Dawn A Hunting for the First Stars in the Universe
... cores, and this is indeed how a star spends the majority of its life. The high temperatures and densities required to sustain fusion are powered by the star’s own selfgravity, which literally squeezes energy out of the core. During this phase of a star’s lifetime, successively heavier elements on th ...
... cores, and this is indeed how a star spends the majority of its life. The high temperatures and densities required to sustain fusion are powered by the star’s own selfgravity, which literally squeezes energy out of the core. During this phase of a star’s lifetime, successively heavier elements on th ...
Galaxy Formation and Evolution Open Problems
... Stellar Halo • 109 old and metal poor stars (Pop.II) • 150 globular clusters (13 Gyr) • <0.2% Galaxy mass, 2% of the light •Dark Halo ...
... Stellar Halo • 109 old and metal poor stars (Pop.II) • 150 globular clusters (13 Gyr) • <0.2% Galaxy mass, 2% of the light •Dark Halo ...
HW #8 Stellar Evolution I Solutions
... rate in the event of fluctuations in the core fusion rate. This is known as a negative feedback cycle. For example, if core fusion rates momentarily increase, then the excess energy generated will increase the temperature of the core and cause the core to expand slightly. The resulting expansion the ...
... rate in the event of fluctuations in the core fusion rate. This is known as a negative feedback cycle. For example, if core fusion rates momentarily increase, then the excess energy generated will increase the temperature of the core and cause the core to expand slightly. The resulting expansion the ...
![David`s Mapping the Heavens[1]](http://s1.studyres.com/store/data/008084229_1-877ead4b57cbb51d927fdcd6d06ce5c8-300x300.png)
Slides from Lecture04
... • Successively fainter stars were catalogued as 2nd magnitude, 3rd magnitude, etc. • Faintest stars (visible to the “naked eye”) were catalogued by Greek astronomers as 6th magnitude stars. • Astronomers continue to use this “magnitude” system, extending it to much fainter objects (that are visible ...
... • Successively fainter stars were catalogued as 2nd magnitude, 3rd magnitude, etc. • Faintest stars (visible to the “naked eye”) were catalogued by Greek astronomers as 6th magnitude stars. • Astronomers continue to use this “magnitude” system, extending it to much fainter objects (that are visible ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.