Unit 11: Stellar Evolution
... The gravitational collapse of a cloud of gas and dust has two important consequences. First, while the cloud is still large, its rotational motion is not obvious. However, as the cloud collapses, it spins faster and faster, much as ice skaters spin faster and faster when they pull in their arms. The ...
... The gravitational collapse of a cloud of gas and dust has two important consequences. First, while the cloud is still large, its rotational motion is not obvious. However, as the cloud collapses, it spins faster and faster, much as ice skaters spin faster and faster when they pull in their arms. The ...
Closed Loop Performance
... At 1000 Hz closed loop we can achieve 65 nm rms error in tower ~95nm “on-sky”. NOTE that this is a linear stretch. This is much better than the 190 nm rms ...
... At 1000 Hz closed loop we can achieve 65 nm rms error in tower ~95nm “on-sky”. NOTE that this is a linear stretch. This is much better than the 190 nm rms ...
Hubble - 15 Years of Discovery
... a planet and it has been named Sedna, after an Inuit goddess. Sedna may be 1500 km in diameter, that’s about three quarters the size of Pluto, but it is so far away that it appears as just a small cluster of pixels even to Hubble. Nevertheless, it is the largest object discovered in the Solar System ...
... a planet and it has been named Sedna, after an Inuit goddess. Sedna may be 1500 km in diameter, that’s about three quarters the size of Pluto, but it is so far away that it appears as just a small cluster of pixels even to Hubble. Nevertheless, it is the largest object discovered in the Solar System ...
Some Examples of Virtual Observatory Enabled Science What Are the Some Distinguishing
... – Radio loud: radio galaxies (RGs) and quasars; F-R types I and II – Radio quiet (but perhaps not entirely radio silent) ...
... – Radio loud: radio galaxies (RGs) and quasars; F-R types I and II – Radio quiet (but perhaps not entirely radio silent) ...
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... 2) Briefly explain what we mean by the statement "The farther away we look in distance, the further back we look in time." Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to t ...
... 2) Briefly explain what we mean by the statement "The farther away we look in distance, the further back we look in time." Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to t ...
Lives of the Stars Lecture 5: Star birth
... easily destroyed. Helium-4 is the only really stable one, so lots of Helium-4 was formed in the next few seconds. But apart from tiny amounts of Lithium-7, no other element can be easily formed. So when the era of fusion ended, about 3½ minutes after the Big Bang, the universe consisted of lots of h ...
... easily destroyed. Helium-4 is the only really stable one, so lots of Helium-4 was formed in the next few seconds. But apart from tiny amounts of Lithium-7, no other element can be easily formed. So when the era of fusion ended, about 3½ minutes after the Big Bang, the universe consisted of lots of h ...
M104: The Sombrero Galaxy
... extending above and below the galaxy’s flat disk. This view also shows that the disks of galaxies are thin. Dust in the galaxy’s wide, flat disk blocks out light from the Sombrero, appearing like a shadow against the bright bulge of stars. In this image, NASA’s Hubble Space Telescope easily resolves ...
... extending above and below the galaxy’s flat disk. This view also shows that the disks of galaxies are thin. Dust in the galaxy’s wide, flat disk blocks out light from the Sombrero, appearing like a shadow against the bright bulge of stars. In this image, NASA’s Hubble Space Telescope easily resolves ...
Exploring Space—The Universe: The Vast
... 7. Based on the content of their reports, each student will create a “What Am I?” presentation and deliver it to the entire class. The students will reveal several facts about their subject matter and ask their classmates to guess what they are describing. Distribute the poster board to students and ...
... 7. Based on the content of their reports, each student will create a “What Am I?” presentation and deliver it to the entire class. The students will reveal several facts about their subject matter and ask their classmates to guess what they are describing. Distribute the poster board to students and ...
Astrophysics Questions (DRAFT)
... evolution. What stars leave (i) white dwarfs, (ii) neutron stars, or (iii) black holes? 58. What is a white dwarf star? Why is the radius of a white dwarf a decreasing function of its mass? What is the basic physics that leads to the upper limit on the mass of a white dwarf (i.e., the Chandrasekhar ...
... evolution. What stars leave (i) white dwarfs, (ii) neutron stars, or (iii) black holes? 58. What is a white dwarf star? Why is the radius of a white dwarf a decreasing function of its mass? What is the basic physics that leads to the upper limit on the mass of a white dwarf (i.e., the Chandrasekhar ...
Far Ultraviolet Spectroscopic Explorer
... Collectively, SNRs can affect star formation and galactic evolution processes. Some massive star SNe appear to be related to Gamma Ray Bursts. Hubble Space Telescope has played a key role in understanding these objects. ...
... Collectively, SNRs can affect star formation and galactic evolution processes. Some massive star SNe appear to be related to Gamma Ray Bursts. Hubble Space Telescope has played a key role in understanding these objects. ...
Rotation Curves:
... (But since the rotation curve is still flat, this is a lower limit.) • For the observed stars in a galaxy, M/L ~3, so between 50% and 90% of a galaxy mass is in dark matter!! – What is it?? We’ll come back to this question later on too. ...
... (But since the rotation curve is still flat, this is a lower limit.) • For the observed stars in a galaxy, M/L ~3, so between 50% and 90% of a galaxy mass is in dark matter!! – What is it?? We’ll come back to this question later on too. ...
Big Bang Theory
... Introduction: Henrietta Leavitt observed Cepheids inside the Small Magellanic Cloud, a star cluster just outside the Milky Way. All of these stars are about the same distance away. Leavitt found that the most luminous Cepheids had the longest periods. By relating each Cepheid’s luminosity to its per ...
... Introduction: Henrietta Leavitt observed Cepheids inside the Small Magellanic Cloud, a star cluster just outside the Milky Way. All of these stars are about the same distance away. Leavitt found that the most luminous Cepheids had the longest periods. By relating each Cepheid’s luminosity to its per ...
A n A n c i e n... How Astronomers Know the Vast Scale of Cosmic Time
... And what we learn from our instruments is that we live in a wonderful universe. No wonder astronomy has inspired artists and poets through the ages, from ancient Greece to today’s television series. Astronomy, the study of the universe, reveals a cosmos that is vast, varied, and beautiful. The sky i ...
... And what we learn from our instruments is that we live in a wonderful universe. No wonder astronomy has inspired artists and poets through the ages, from ancient Greece to today’s television series. Astronomy, the study of the universe, reveals a cosmos that is vast, varied, and beautiful. The sky i ...
- IRSF: Past and Future
... associated with accretion onto dense objects. Over the last decade or so, optical imaging surveys, like OGLE, CRTS, MASTER and ASAS-SN, have increased the rate of discoveries of many different types of optical transients, including CVs, SNe, GRB afterglows, eruptive variables and flaring blazars. Th ...
... associated with accretion onto dense objects. Over the last decade or so, optical imaging surveys, like OGLE, CRTS, MASTER and ASAS-SN, have increased the rate of discoveries of many different types of optical transients, including CVs, SNe, GRB afterglows, eruptive variables and flaring blazars. Th ...
Today in Astronomy 102: observations of stellar
... The X-ray source has a stellar companion, a star rather similar to the Sun (about 1.1 M); the X-ray source and the visible star revolve around each other with a period of 2.92 days. Their distance from us is measured to be 6500 light years. A stroke of luck: it is an eclipsing system, so the or ...
... The X-ray source has a stellar companion, a star rather similar to the Sun (about 1.1 M); the X-ray source and the visible star revolve around each other with a period of 2.92 days. Their distance from us is measured to be 6500 light years. A stroke of luck: it is an eclipsing system, so the or ...
Astronomy Astrophysics Circumstellar emission in Be/X-ray binaries of the Magellanic
... need a set of programme stars with well-known distances and interstellar reddenings as well as good determinations of the spectral types. In principle we could choose Be/X-ray binaries in well-studied open clusters and follow an approach similar to the one used by Fabregat & Torrejón (1998). Unfortu ...
... need a set of programme stars with well-known distances and interstellar reddenings as well as good determinations of the spectral types. In principle we could choose Be/X-ray binaries in well-studied open clusters and follow an approach similar to the one used by Fabregat & Torrejón (1998). Unfortu ...
Classification_of_Stars_By_Luminosity
... Apparent magnitude • Apparent magnitude is not necessarily related to the amount of light actually produced by the star but is simply a measure of how bright it appears to be from Earth. • (Some bright stars are simply close neighbours while other giant stars may appear equally bright but are also ...
... Apparent magnitude • Apparent magnitude is not necessarily related to the amount of light actually produced by the star but is simply a measure of how bright it appears to be from Earth. • (Some bright stars are simply close neighbours while other giant stars may appear equally bright but are also ...
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... 2) Briefly explain what we mean by the statement "The farther away we look in distance, the further back we look in time." Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to t ...
... 2) Briefly explain what we mean by the statement "The farther away we look in distance, the further back we look in time." Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to t ...
Solutions to Homework #4, AST 203, Spring 2012
... rotation of the neutron star will be much shorter, as we expect. Substituting numbers, RNS /RCO = 10km/(0.5R ) ≈ 2×10−5 . The period is then PNS = (2×10−5 )2 ×30days ≈ 1 millisecond. This number is actually near the limit of how fast a neutron star can rotate. From observations of radio pulsars we ...
... rotation of the neutron star will be much shorter, as we expect. Substituting numbers, RNS /RCO = 10km/(0.5R ) ≈ 2×10−5 . The period is then PNS = (2×10−5 )2 ×30days ≈ 1 millisecond. This number is actually near the limit of how fast a neutron star can rotate. From observations of radio pulsars we ...
Astronomy Astrophysics First detection of the field star overdensity in the Perseus... &
... or EC method (see Fig. 1). This sample contains stars with more accurate SPP data, but has fewer statistics owing to the lack of stars rejected during the cleaning process. From now on we will distinguish between the subsamples containing the stars in the inner sky area (in suffix), from those where t ...
... or EC method (see Fig. 1). This sample contains stars with more accurate SPP data, but has fewer statistics owing to the lack of stars rejected during the cleaning process. From now on we will distinguish between the subsamples containing the stars in the inner sky area (in suffix), from those where t ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.