Star Formation
... Massive newborn stars are indicated by the arrows. Note that some (2, 3, & 4) are hidden to visible light. Arrows 1 and 5 indicate a compact cluster of bright young stars. Sources 6 & 7 may be due to outflow jets from the cluster 5. ...
... Massive newborn stars are indicated by the arrows. Note that some (2, 3, & 4) are hidden to visible light. Arrows 1 and 5 indicate a compact cluster of bright young stars. Sources 6 & 7 may be due to outflow jets from the cluster 5. ...
August 2015 - Shasta Astronomy Club
... so-called ultracompact dwarf galaxies while sifting through opensource archives of astronomy observations by several different observatories as undergraduates at San Jose State University in California. They also created a video simulation depicting how such dense galaxies can form with a supermassi ...
... so-called ultracompact dwarf galaxies while sifting through opensource archives of astronomy observations by several different observatories as undergraduates at San Jose State University in California. They also created a video simulation depicting how such dense galaxies can form with a supermassi ...
Summary: Stellar Distances
... Stellar Colors & Luminosities Color and Temperature The color of a star is related to its surface temperature. “surface” = “photosphere” Observed color is almost independent of the star’s distance. Interstellar dust makes stars look redder over long distances Temperatures can also be inferred from ...
... Stellar Colors & Luminosities Color and Temperature The color of a star is related to its surface temperature. “surface” = “photosphere” Observed color is almost independent of the star’s distance. Interstellar dust makes stars look redder over long distances Temperatures can also be inferred from ...
The Milky Way Galaxy
... velocities of those globular clusters were ~250 km/s, much higher than the mass of the smaller Kapteyn galaxy model would require. So the galaxy must contain more stars (and mass) than Kapteyn originally thought in order to keep the star clusters from flying off. ...
... velocities of those globular clusters were ~250 km/s, much higher than the mass of the smaller Kapteyn galaxy model would require. So the galaxy must contain more stars (and mass) than Kapteyn originally thought in order to keep the star clusters from flying off. ...
MilkyWay
... velocities of those globular clusters were ~250 km/s, much higher than the mass of the smaller Kapteyn galaxy model would require. So the galaxy must contain more stars (and mass) than Kapteyn originally thought in order to keep the star clusters from flying off. ...
... velocities of those globular clusters were ~250 km/s, much higher than the mass of the smaller Kapteyn galaxy model would require. So the galaxy must contain more stars (and mass) than Kapteyn originally thought in order to keep the star clusters from flying off. ...
Chapter 8 - TeacherWeb
... atmosphere expands. Red giants can be 10X bigger than the sun and supergiants can be 100X bigger. ...
... atmosphere expands. Red giants can be 10X bigger than the sun and supergiants can be 100X bigger. ...
Recap: High Mass Stars
... years Stars away! • From ½ all the way down to 0.075% of the Sun’s mass • Burn cool, less than 3500 K. Dim light. • Can live a REALLY long time. 10,000,000,000,000 years? • Our nearest star neighbor is Proxima Centauri, a red dwarf. • Most numerous stars in the entire Universe! ...
... years Stars away! • From ½ all the way down to 0.075% of the Sun’s mass • Burn cool, less than 3500 K. Dim light. • Can live a REALLY long time. 10,000,000,000,000 years? • Our nearest star neighbor is Proxima Centauri, a red dwarf. • Most numerous stars in the entire Universe! ...
Study Guide for 3RD Astronomy Exam
... and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main sequence lifetime. Unit 63: Giant Stars Describe how shell f ...
... and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main sequence lifetime. Unit 63: Giant Stars Describe how shell f ...
SR Stellar Properties
... The Hertzsprung-Russell diagram provides a way to group similar stars. The H-R diagram is a graph of absolute magnitude, sometimes called absolute brightness, actual brightness or luminosity, and temperature. In this activity, students will construct an H-R diagram using data on the 20 stars that ar ...
... The Hertzsprung-Russell diagram provides a way to group similar stars. The H-R diagram is a graph of absolute magnitude, sometimes called absolute brightness, actual brightness or luminosity, and temperature. In this activity, students will construct an H-R diagram using data on the 20 stars that ar ...
Stellar Evolution
... cycles of stars. Most stars fall within a band that runs diagonally through the middle of the H-R diagram. These stars are main sequence stars. ...
... cycles of stars. Most stars fall within a band that runs diagonally through the middle of the H-R diagram. These stars are main sequence stars. ...
Tour the sky`s reddest stars
... The standard spectral classes assign letters to stars based on their temperatures. From hottest to coolest, the letters run O, B, A, F, G, K, and M. Since that system debuted, however, astronomers have classified even cooler stars. And the coolest of all are carbon stars, designated C. Carbon stars ...
... The standard spectral classes assign letters to stars based on their temperatures. From hottest to coolest, the letters run O, B, A, F, G, K, and M. Since that system debuted, however, astronomers have classified even cooler stars. And the coolest of all are carbon stars, designated C. Carbon stars ...
A Star is “Born,” and then How Will it Move
... Young (Embedded) Clusters: Very young (<10 Myr-old) groups of young stars that form together. Future binding depends on cluster mass & velocity, seems that 90% dissolve before ~10 Myr (Lada & Lada 2003). When they unbind but are still seen to move together, they’re known as a “stellar association.” ...
... Young (Embedded) Clusters: Very young (<10 Myr-old) groups of young stars that form together. Future binding depends on cluster mass & velocity, seems that 90% dissolve before ~10 Myr (Lada & Lada 2003). When they unbind but are still seen to move together, they’re known as a “stellar association.” ...
Directed Reading A
... _____ 18. left side of modern H-R diagram 19. Place these stars in order from earliest in life cycle to oldest in life cycle: red giant, white dwarf, main-sequence star. _______________________________________________________________ _______________________________________________________________ __ ...
... _____ 18. left side of modern H-R diagram 19. Place these stars in order from earliest in life cycle to oldest in life cycle: red giant, white dwarf, main-sequence star. _______________________________________________________________ _______________________________________________________________ __ ...
Some interesting geometric facts about eclipsing binaries (see if you
... Some interesting geometric facts about eclipsing binaries (see if you can prove these): The probability of a binary being properly oriented in space for us to observe it as an eclipsing system becomes progressively smaller as the distance between the two stars increases. It turns out that no visual ...
... Some interesting geometric facts about eclipsing binaries (see if you can prove these): The probability of a binary being properly oriented in space for us to observe it as an eclipsing system becomes progressively smaller as the distance between the two stars increases. It turns out that no visual ...
Calculating Main Sequence Lifetimes
... If the stellar mass is not enough to light new thermonuclear reaction beyond the Helium burning, it ‘dies’ as a white dwarfs of Helium. ...
... If the stellar mass is not enough to light new thermonuclear reaction beyond the Helium burning, it ‘dies’ as a white dwarfs of Helium. ...
Stages of stars - University of Dayton
... gaseous shell, this gas that surrounds the core is called a Planetary Nebula. ...
... gaseous shell, this gas that surrounds the core is called a Planetary Nebula. ...
Radio-quiet Isolated Neutron Stars
... Detected in the RASS between 1990/09/14~1990/10/02. Identified with the 1992/10/16 PSPC data. No variability at levels greater than ~1% in 1hr, or <30% on timescale up to 15 years. ...
... Detected in the RASS between 1990/09/14~1990/10/02. Identified with the 1992/10/16 PSPC data. No variability at levels greater than ~1% in 1hr, or <30% on timescale up to 15 years. ...
Astronomy news
... The accurate parallactic distance (500 Lyrs) of RX J1856 which was supplied by HST has allowed astronomers to use the brightness to estimate its radius. The estimated radius came out to be smaller than 10 km and this was taken as possible evidence that RX J1856 was an exotic object, known as a quark ...
... The accurate parallactic distance (500 Lyrs) of RX J1856 which was supplied by HST has allowed astronomers to use the brightness to estimate its radius. The estimated radius came out to be smaller than 10 km and this was taken as possible evidence that RX J1856 was an exotic object, known as a quark ...
doc
... 19.17 (open cluster) and 19.18 (globular cluster) on p. 519 of your book, and understand clearly how we know that one was “just born” recently (about 100 million years ago), while the other must be extremely old, about 10 billion years. Can you now guess why so many globular clusters have about the ...
... 19.17 (open cluster) and 19.18 (globular cluster) on p. 519 of your book, and understand clearly how we know that one was “just born” recently (about 100 million years ago), while the other must be extremely old, about 10 billion years. Can you now guess why so many globular clusters have about the ...
October 2013
... 'Coalsack', a remarkable dark cloud of dust blocking almost all light from stars behind it, spills over into Musca from the Southern Cross. This cloud is about 550 light years away, 60 light years across and weighs about 3500 times as much as our ...
... 'Coalsack', a remarkable dark cloud of dust blocking almost all light from stars behind it, spills over into Musca from the Southern Cross. This cloud is about 550 light years away, 60 light years across and weighs about 3500 times as much as our ...
answers
... distant objects ever found. All of the objects are galaxies of stars except for E, which is a single nearby star. Which object is more luminous? A) E B) F C) they are about the same B) The two objects look equally bright, but are very different. The star is much closer and much less luminous. The ga ...
... distant objects ever found. All of the objects are galaxies of stars except for E, which is a single nearby star. Which object is more luminous? A) E B) F C) they are about the same B) The two objects look equally bright, but are very different. The star is much closer and much less luminous. The ga ...
Sample multiple choice questions for Exam 2
... 25. Why do massive stars run out of hydrogen in their cores faster than less massive stars? a) Their hydrogen fuses faster because of greater temperatures inside. b) There is less hydrogen in their cores. c) The cores of less massive stars contain a greater percentage of helium, which slows hydrogen ...
... 25. Why do massive stars run out of hydrogen in their cores faster than less massive stars? a) Their hydrogen fuses faster because of greater temperatures inside. b) There is less hydrogen in their cores. c) The cores of less massive stars contain a greater percentage of helium, which slows hydrogen ...
ASTRONOMY WEBQUEST…… EXPLORE THE UNIVERSE
... http://outreach.atnf.csiro.au/education/everyone/pulsars/ ...
... http://outreach.atnf.csiro.au/education/everyone/pulsars/ ...
Astronomy 1020 Exam 4 Review Questions
... shape of the curve in the outer regions of the Galaxy suggest about the halo? When compared to the light distribution, what else can you say about the halo? How long does it take the Sun to complete one orbit about the center of the Galaxy? As such, what is the length of its galactic year? How old i ...
... shape of the curve in the outer regions of the Galaxy suggest about the halo? When compared to the light distribution, what else can you say about the halo? How long does it take the Sun to complete one orbit about the center of the Galaxy? As such, what is the length of its galactic year? How old i ...
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.