Distance
... If stars are too far away, the parallax can be too small to measure accurately. The smallest parallax measurable from the ground is about 0.01‐arcsec • Measure distances out to ~100 pc • But, only a few hundred stars this close ...
... If stars are too far away, the parallax can be too small to measure accurately. The smallest parallax measurable from the ground is about 0.01‐arcsec • Measure distances out to ~100 pc • But, only a few hundred stars this close ...
life cycles of stars
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
Stellar Evolution 1
... into Helium in core of a star? 6. As a result of the increase in the rate of nuclear energy generation, what happens to the Luminosity a) It increases b) It remains the same (until the pressure outside the core builds up enough to make the surrounding envelope expand which reduces the insulation and ...
... into Helium in core of a star? 6. As a result of the increase in the rate of nuclear energy generation, what happens to the Luminosity a) It increases b) It remains the same (until the pressure outside the core builds up enough to make the surrounding envelope expand which reduces the insulation and ...
20_LectureOutline
... This double cluster, h and chi Persei, must be quite young—its H-R diagram is that of a newborn cluster. Its age cannot be more than about 10 million years. ...
... This double cluster, h and chi Persei, must be quite young—its H-R diagram is that of a newborn cluster. Its age cannot be more than about 10 million years. ...
Unit 3 - Lesson 8.9 Life of Stars Challenge
... These coloured Super Giants have luminosities often 1,000,000X greater than the Sun The explosive death of a star A cloud of hydrogen gas and dust in space. When the gravitational and pressure forces within the initial cloud become unbalanced, the cloud collapses and breaks into small fragments. The ...
... These coloured Super Giants have luminosities often 1,000,000X greater than the Sun The explosive death of a star A cloud of hydrogen gas and dust in space. When the gravitational and pressure forces within the initial cloud become unbalanced, the cloud collapses and breaks into small fragments. The ...
The Origin, Structure, and Evolution of the Stars
... the evolutionary tracks of stars off the main-sequence and also gives the time spent as main-sequence stars for stars in different regions of the H-R diagram. Our calculations indicate that the more massive stars “burn” their fuel so rapidly they cannot last very long. Some of these bright stars mus ...
... the evolutionary tracks of stars off the main-sequence and also gives the time spent as main-sequence stars for stars in different regions of the H-R diagram. Our calculations indicate that the more massive stars “burn” their fuel so rapidly they cannot last very long. Some of these bright stars mus ...
Chapter 10: The Interstellar Medium - Otto
... The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful objects in the sky. We are interested in the interstellar medium because a) dense interstellar clouds are the birth place of stars b) Dark clouds alter and absorb the l ...
... The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful objects in the sky. We are interested in the interstellar medium because a) dense interstellar clouds are the birth place of stars b) Dark clouds alter and absorb the l ...
Zero Age Main Sequence (ZAMS)
... • How the helium burning starts depends on the mass of the star. • In high mass stars (>2M⁄ ) helium burning starts gradually as ...
... • How the helium burning starts depends on the mass of the star. • In high mass stars (>2M⁄ ) helium burning starts gradually as ...
LIFE CYCLE OF STARS
... Cool at the end of the Red Giant stage faster than larger stars, so they begin to shed its gases outside its core forming a planetary nebula . The center of the small star then begins to cool to become a white dwarf and cools more to become a black dwarf. Large Stars Larger stars are hotter th ...
... Cool at the end of the Red Giant stage faster than larger stars, so they begin to shed its gases outside its core forming a planetary nebula . The center of the small star then begins to cool to become a white dwarf and cools more to become a black dwarf. Large Stars Larger stars are hotter th ...
13.1 Introduction 13.2 The Red Giant Branch
... results in an explosive start of the fusion known as the “Helium Flash”. The ignition of He-fusion raises the temperature of the core, but this does not raise the pressure, because in a degenerate gas P 6= f (T ). Thus, as T increases the core does not expand, and the density remains the same. As we ...
... results in an explosive start of the fusion known as the “Helium Flash”. The ignition of He-fusion raises the temperature of the core, but this does not raise the pressure, because in a degenerate gas P 6= f (T ). Thus, as T increases the core does not expand, and the density remains the same. As we ...
Xiao Yang Xia
... (2) Star formation rate and accretion rate onto the central BH in IR QSOs at low redshift follow Mbulge- MBH relation, i.e., the ratio of the star formation rate and the accretion rate is about several hundred for IR QSOs, but decreases with the central black hole mass. This shows that the tight cor ...
... (2) Star formation rate and accretion rate onto the central BH in IR QSOs at low redshift follow Mbulge- MBH relation, i.e., the ratio of the star formation rate and the accretion rate is about several hundred for IR QSOs, but decreases with the central black hole mass. This shows that the tight cor ...
chapter 7 review questions
... 10. Hydrogen lines are weak in the spectra of hot stars because many of the hydrogen atoms have their electrons in levels above the second level. ...
... 10. Hydrogen lines are weak in the spectra of hot stars because many of the hydrogen atoms have their electrons in levels above the second level. ...
Oct - Seattle Astronomical Society
... The galaxy appears to be a merger, a “train wreck” of two or more galaxies crashing together. The crash is what produces the baby boom. Clouds of interstellar gas within the two galaxies press against one another and collapse to form stars, dozens to hundreds at a time. This isn’t the first time ast ...
... The galaxy appears to be a merger, a “train wreck” of two or more galaxies crashing together. The crash is what produces the baby boom. Clouds of interstellar gas within the two galaxies press against one another and collapse to form stars, dozens to hundreds at a time. This isn’t the first time ast ...
The Formation of Massive Star Systems by Accretion
... radiation pressure produced no noticeable effects. After ~20,000 years, the disk became gravitationally unstable and developed a pronounced twoarmed spiral that transported angular momentum efficiently (Fig. 1B) (24). Accretion onto the protostar continued smoothly. Accretion, unimpeded by radiation ...
... radiation pressure produced no noticeable effects. After ~20,000 years, the disk became gravitationally unstable and developed a pronounced twoarmed spiral that transported angular momentum efficiently (Fig. 1B) (24). Accretion onto the protostar continued smoothly. Accretion, unimpeded by radiation ...
Neutron Stars PowerPoint
... The two stars were of substantially different mass The high-mass star evolved quickly & died in a supernova The low -mass star survived to the red giant phase The low -mass star over-fills its Roche lobe Mass transfer “spins up” the companion neutron star ...
... The two stars were of substantially different mass The high-mass star evolved quickly & died in a supernova The low -mass star survived to the red giant phase The low -mass star over-fills its Roche lobe Mass transfer “spins up” the companion neutron star ...
O star
... (1) temperature and (2) the density or pressure (pressure is proportional to density times temperature). A higher density at the same temperature leads to a lower ionizationrecombination goes faster- while the converse is true at lower density. Because supergiants are so large compared to dwarfs, th ...
... (1) temperature and (2) the density or pressure (pressure is proportional to density times temperature). A higher density at the same temperature leads to a lower ionizationrecombination goes faster- while the converse is true at lower density. Because supergiants are so large compared to dwarfs, th ...
ASTRONOMY 301 EXAMPLES OF TEST
... water, you would see the Sun as a brilliant light above the water. (B) The inside of a refrigerator would look black, but people would glow. (C) A roaring campfire would look bright. (D) Steam would be a bright cloud compared to your surroundings on a pleasant summer day. 34. Stellar parallax is (A) ...
... water, you would see the Sun as a brilliant light above the water. (B) The inside of a refrigerator would look black, but people would glow. (C) A roaring campfire would look bright. (D) Steam would be a bright cloud compared to your surroundings on a pleasant summer day. 34. Stellar parallax is (A) ...