PDF Version
... varies with the star’s intrinsic brightness. The star’s apparent brightness, which is the brightness that we can see ourselves, is equal to the intrinsic brightness divided by the square of the distance from us to the star. Astronomers used Cepheid variables in a nearby galaxy, which are all about t ...
... varies with the star’s intrinsic brightness. The star’s apparent brightness, which is the brightness that we can see ourselves, is equal to the intrinsic brightness divided by the square of the distance from us to the star. Astronomers used Cepheid variables in a nearby galaxy, which are all about t ...
Constellations
... the people of other cultures, even though they were all looking at the same stars in the night sky. Interestingly, though, different cultures often made the same basic groupings of stars, despite widely varying interpretations of what they saw. For example, the group of seven stars usually known in ...
... the people of other cultures, even though they were all looking at the same stars in the night sky. Interestingly, though, different cultures often made the same basic groupings of stars, despite widely varying interpretations of what they saw. For example, the group of seven stars usually known in ...
doc
... Bonus marks for extra labels. c. What is the galaxy’s classification on the Hubble sequence (e.g., Sa, SBc, etc.)? If you can’t find the classification in the literature, make your best guess from the picture and explain your reasoning. Bonus mark for discussing whether any classification found in t ...
... Bonus marks for extra labels. c. What is the galaxy’s classification on the Hubble sequence (e.g., Sa, SBc, etc.)? If you can’t find the classification in the literature, make your best guess from the picture and explain your reasoning. Bonus mark for discussing whether any classification found in t ...
Stars Part 1
... Two 3He nuclei may eventually (within ten thousand years) find each other. 3He ...
... Two 3He nuclei may eventually (within ten thousand years) find each other. 3He ...
Power-point slides for Lecture 2
... In massive stars, mass loss is chiefly a consequence of radiation pressure on grains and atoms. In quite massive stars, shocks and turbulence may be very important. ...
... In massive stars, mass loss is chiefly a consequence of radiation pressure on grains and atoms. In quite massive stars, shocks and turbulence may be very important. ...
www.esf.org - European Science Foundation
... different environments? Is there a lower limit to the IMF? Can a molecular cloud sustain or not the production of stars for a period of time comparable to its lifetime (>10Myr) and much longer than the typical free-fall time of dense gas (<1Myr)? Currently there is no consensus on the prevalence of ...
... different environments? Is there a lower limit to the IMF? Can a molecular cloud sustain or not the production of stars for a period of time comparable to its lifetime (>10Myr) and much longer than the typical free-fall time of dense gas (<1Myr)? Currently there is no consensus on the prevalence of ...
astronomy - Scioly.org
... 48. Variable stars are stars in which the _______ changes over time. A. Size B. Color C. Shape D. brightness 49. A planet orbits the Sun at 3 AU. How long (in years) does it take to orbit the Sun? (Hint: Find its period using Kepler’s Third Law. The Earth is at 1 AU.) [Used as tie breaker] 50. Descr ...
... 48. Variable stars are stars in which the _______ changes over time. A. Size B. Color C. Shape D. brightness 49. A planet orbits the Sun at 3 AU. How long (in years) does it take to orbit the Sun? (Hint: Find its period using Kepler’s Third Law. The Earth is at 1 AU.) [Used as tie breaker] 50. Descr ...
MS Word
... stars against their spectral types. It is named after Hertzprung and Russell who discovered this relation. You will discover that there are many different kinds of stars of different brightness, surface temperature and size. ...
... stars against their spectral types. It is named after Hertzprung and Russell who discovered this relation. You will discover that there are many different kinds of stars of different brightness, surface temperature and size. ...
![[WC 6] nucleus with other emission-lines nuclei of planetary nebulae](http://s1.studyres.com/store/data/004159324_1-0806f9baff29e598ec0946db112c7fad-300x300.png)
NASA`s Spitzer Images Out-of-This
... eventually enter a more dormant state like our Milky Way black hole." The ring around the black hole is bursting with new star formation. An inflow of material toward the central bar of the galaxy is causing the ring to light up with new stars. "The ring itself is a fascinating object worthy of stud ...
... eventually enter a more dormant state like our Milky Way black hole." The ring around the black hole is bursting with new star formation. An inflow of material toward the central bar of the galaxy is causing the ring to light up with new stars. "The ring itself is a fascinating object worthy of stud ...
26.4 Groups of Stars
... The Milky Way’s flattened disk shape is caused by its rotation. The sun takes about 220 million years to complete one orbit around the galaxy’s center. Recent evidence suggests that there is a massive black hole at our galaxy’s center. Stars are forming in the galaxy's spiral arms. ...
... The Milky Way’s flattened disk shape is caused by its rotation. The sun takes about 220 million years to complete one orbit around the galaxy’s center. Recent evidence suggests that there is a massive black hole at our galaxy’s center. Stars are forming in the galaxy's spiral arms. ...
Catching Andromeda`s Light
... Andromeda’s spiral arms, he thought they might also trace the Milky Way’s spiral arms. So in 1951, Morgan mapped the locations of all the red clouds of gas he and his colleagues could find. He discovered that the gas clouds lined up along spiral arms, indicating that we live in a spiral galaxy. Why ...
... Andromeda’s spiral arms, he thought they might also trace the Milky Way’s spiral arms. So in 1951, Morgan mapped the locations of all the red clouds of gas he and his colleagues could find. He discovered that the gas clouds lined up along spiral arms, indicating that we live in a spiral galaxy. Why ...
preliminary version - University of Exeter
... The most efficient method of determining large numbers of periods for young stars is via photometric monitoring. Unfortunately, this method has proved insensitive to periods amongst CTTs in the past, largely due to the irregular variability shown by CTTs[2,3]. This bias against CTTs is a major probl ...
... The most efficient method of determining large numbers of periods for young stars is via photometric monitoring. Unfortunately, this method has proved insensitive to periods amongst CTTs in the past, largely due to the irregular variability shown by CTTs[2,3]. This bias against CTTs is a major probl ...
Neutron Stars and Pulsars
... • Explanation: Neutron star with a normal star companion. • Close enough for normal star material to pass through the inner Lagrangian point, form a disk around the neutron star, and accrete onto it. • As the mixture of hydrogen and helium accumulates on the surface of the neutron star, the hydrogen ...
... • Explanation: Neutron star with a normal star companion. • Close enough for normal star material to pass through the inner Lagrangian point, form a disk around the neutron star, and accrete onto it. • As the mixture of hydrogen and helium accumulates on the surface of the neutron star, the hydrogen ...
PowerPoint
... The first law allows one to apply a turning point theorem (Sorkin 1981) to sequence of binary equilibria. The theorem shows that on one side of a turning point in M at fixed J or in J and fixed baryon mass M0, the sequence is unstable. The side on which M is smaller is more tightly bound - the stabl ...
... The first law allows one to apply a turning point theorem (Sorkin 1981) to sequence of binary equilibria. The theorem shows that on one side of a turning point in M at fixed J or in J and fixed baryon mass M0, the sequence is unstable. The side on which M is smaller is more tightly bound - the stabl ...
Spectral_Analysis
... Almost all the lines in light from extraterrestrial sources were attributed to known elements, however, some new lines also appeared in the solar spectrum. In 1868, astronomers realised that those lines must correspond to a previously unknown element. It was given the name helium, after the Greek wo ...
... Almost all the lines in light from extraterrestrial sources were attributed to known elements, however, some new lines also appeared in the solar spectrum. In 1868, astronomers realised that those lines must correspond to a previously unknown element. It was given the name helium, after the Greek wo ...
Measuring Stars` Properties - Test 1 Study Guide
... • For a few close, big stars, they can be seen in a telescope as non-point objects • Measure angular size; if know distance then get size of star Example: Betelgeuse 300 times larger radius than the Sun • If further away but a binary star, get size of stars when they eclipse each other ! length o ...
... • For a few close, big stars, they can be seen in a telescope as non-point objects • Measure angular size; if know distance then get size of star Example: Betelgeuse 300 times larger radius than the Sun • If further away but a binary star, get size of stars when they eclipse each other ! length o ...
Solution Set
... There are several possible signals that would prove it is not a black hole, but instead a neutron star. The detection of a pulsar would indicate a spinning neutron star. X-‐ray bursts, from ...
... There are several possible signals that would prove it is not a black hole, but instead a neutron star. The detection of a pulsar would indicate a spinning neutron star. X-‐ray bursts, from ...
Galactic Encounters: The Dynamics of Mergers and Satellite Accretion
... galaxies merge, direct hits of stars are very unlikely. This shouldn’t be surprising, considering how small the fraction of the area filled by stars in a galaxy is. For the solar neighbourhood we typically have 20 stars/pc3 and the radius of each star is about 0.2Rsun on average. So the fractional a ...
... galaxies merge, direct hits of stars are very unlikely. This shouldn’t be surprising, considering how small the fraction of the area filled by stars in a galaxy is. For the solar neighbourhood we typically have 20 stars/pc3 and the radius of each star is about 0.2Rsun on average. So the fractional a ...
Powerpoint file
... • Most challenging observational technique due to proximity, contrast levels and atmospheric effects (AO, coronagraphy,..) • Candidates appeared at large (~100 AU) separations and mass determination is limited by reliability of evolutionary models (if no other information) • More robust detections ( ...
... • Most challenging observational technique due to proximity, contrast levels and atmospheric effects (AO, coronagraphy,..) • Candidates appeared at large (~100 AU) separations and mass determination is limited by reliability of evolutionary models (if no other information) • More robust detections ( ...
s-process
... Significant production of r-process elements began when the metallicity of the Galaxy reached [Fe/H] = -3. The heavy n-capture elements were formed predominantly by the r-process at metallicities below [Fe/H] = -2.1. Elements from the s-process appear at a metallicity of [Fe/H] = -2.1, when low-mass ...
... Significant production of r-process elements began when the metallicity of the Galaxy reached [Fe/H] = -3. The heavy n-capture elements were formed predominantly by the r-process at metallicities below [Fe/H] = -2.1. Elements from the s-process appear at a metallicity of [Fe/H] = -2.1, when low-mass ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.