Notes for Class 7, March 2
... • Example 7: A gas with a volume of 3 quarts and a pressure of 4 atmospheres beforehand is expanded to a volume of 6 quarts. Find its pressure after the expansion. • Example 8: A gas with an earlier pressure of 2 inches of Mercury and a volume of 6 cubic feet is compressed to a pressure of 3 inches ...
... • Example 7: A gas with a volume of 3 quarts and a pressure of 4 atmospheres beforehand is expanded to a volume of 6 quarts. Find its pressure after the expansion. • Example 8: A gas with an earlier pressure of 2 inches of Mercury and a volume of 6 cubic feet is compressed to a pressure of 3 inches ...
The Recent Star Formation Histories of M81 Group Dwarf Irregular
... The ability to translate resolved stellar populations into star formation histories (SFHs) has become an increasingly powerful method for understanding how star formation (SF) shapes galaxy evolution (e.g., Gallart et al. 2005). The power of the Hubble Space Telescope (HST) is truly being realized a ...
... The ability to translate resolved stellar populations into star formation histories (SFHs) has become an increasingly powerful method for understanding how star formation (SF) shapes galaxy evolution (e.g., Gallart et al. 2005). The power of the Hubble Space Telescope (HST) is truly being realized a ...
Stars
... • While stars are in the main sequence, they are fusing hydrogen in their cores. As stars evolve off the main sequence, they begin to fuse helium in their cores and burn hydrogen around the core edges. ...
... • While stars are in the main sequence, they are fusing hydrogen in their cores. As stars evolve off the main sequence, they begin to fuse helium in their cores and burn hydrogen around the core edges. ...
Satellities - stoweschools.com
... Bipolar Star System Two stars 8x1010m apart rotate about a point 4x1010 m from each other in a circular path in 12.6 years. The two stars have the same mass. What is the mass of the stars? Fg causes the centripetal acceleration therefore Fg = Fc ...
... Bipolar Star System Two stars 8x1010m apart rotate about a point 4x1010 m from each other in a circular path in 12.6 years. The two stars have the same mass. What is the mass of the stars? Fg causes the centripetal acceleration therefore Fg = Fc ...
Investigate Planets, Stars, Galaxies, and the Universe
... between objects in the universe. But since the universe is so large, it is difficult to truly understand these gaps. One way to make this mental leap is to use scale models. By comparing planets, our solar system and even our galaxy with the everyday things, the unimaginable distances in the cosmos ...
... between objects in the universe. But since the universe is so large, it is difficult to truly understand these gaps. One way to make this mental leap is to use scale models. By comparing planets, our solar system and even our galaxy with the everyday things, the unimaginable distances in the cosmos ...
The Spitzer/GLIMPSE Surveys - UW-Madison Astronomy
... crash into the ambient interstellar medium and excite NIR line emission. NIR H2 narrow-band images and ISO spectra show that the extended 4.5 μm emission of the massive DR21 outflow is due to shocked H2 (Davis et al. 2007; Smith et al. 2006, and references therein); Smith et al. (2006) do not detect ...
... crash into the ambient interstellar medium and excite NIR line emission. NIR H2 narrow-band images and ISO spectra show that the extended 4.5 μm emission of the massive DR21 outflow is due to shocked H2 (Davis et al. 2007; Smith et al. 2006, and references therein); Smith et al. (2006) do not detect ...
instructor notes stellar evolution, star clusters
... During the Hayashi track phases newly-formed stars are thoroughly mixed, since convection is the most efficient way of releasing energy from the object. At some stage (earlier for massive stars) the contracting star slows its contraction as the mode of energy escape changes from convective transpor ...
... During the Hayashi track phases newly-formed stars are thoroughly mixed, since convection is the most efficient way of releasing energy from the object. At some stage (earlier for massive stars) the contracting star slows its contraction as the mode of energy escape changes from convective transpor ...
instructor notes stellar evolution, star clusters
... During the Hayashi track phases newly-formed stars are thoroughly mixed, since convection is the most efficient way of releasing energy from the object. At some stage (earlier for massive stars) the contracting star slows its contraction as the mode of energy escape changes from convective transpor ...
... During the Hayashi track phases newly-formed stars are thoroughly mixed, since convection is the most efficient way of releasing energy from the object. At some stage (earlier for massive stars) the contracting star slows its contraction as the mode of energy escape changes from convective transpor ...
Chapter 12 Lecture 2
... What have we learned? • What are the life stages of a low-mass star? • A low-mass star spends most of its life generating energy by fusing hydrogen in its core. Then it becomes a red giant, with a hydrogen shell burning around an inert helium core. Next comes helium core burning, followed by doub ...
... What have we learned? • What are the life stages of a low-mass star? • A low-mass star spends most of its life generating energy by fusing hydrogen in its core. Then it becomes a red giant, with a hydrogen shell burning around an inert helium core. Next comes helium core burning, followed by doub ...
LET THE STARS GET IN YOUR EYES SKY MOTIONS
... known as the primary mirror. It bends or reflects the light striking it's surface back to where it can be focused. The place where the object comes into focus is known as the focal point. The distance between the primary mirror and the focal point determines the telescope's focal length. The focal l ...
... known as the primary mirror. It bends or reflects the light striking it's surface back to where it can be focused. The place where the object comes into focus is known as the focal point. The distance between the primary mirror and the focal point determines the telescope's focal length. The focal l ...
6.1 Introduction
... with a mass of 107 M ) is unique among Galactic globular clusters in showing two distinct populations of stars, a bluer population and a redder one, with quite distinct main sequences in the colour-magnitude diagram. The origin of these two populations is still unclear. This figure compares a small ...
... with a mass of 107 M ) is unique among Galactic globular clusters in showing two distinct populations of stars, a bluer population and a redder one, with quite distinct main sequences in the colour-magnitude diagram. The origin of these two populations is still unclear. This figure compares a small ...
The Helium Flash • When the temperature of a stellar core reaches T
... (∼ 0.4 M⊙ ) appear near the base of the red giant branch. The star’s total mass or core mass does not affect the star’s effective temperature, except through determining the envelope mass. • Both helium-core burning and hydrogen shell-burning contribute to the luminosity of a horizontal branch star. I ...
... (∼ 0.4 M⊙ ) appear near the base of the red giant branch. The star’s total mass or core mass does not affect the star’s effective temperature, except through determining the envelope mass. • Both helium-core burning and hydrogen shell-burning contribute to the luminosity of a horizontal branch star. I ...
Carbon Stars - The OzSky Star Safari
... area of the HR diagram that we call an 'instability strip' or an 'instability region'. When the star is in this area of the diagram it will become a variable star, one that varies in brightness over time.“ • “Mira stars are red giants (which began as low mass stars), with a temperature less than ...
... area of the HR diagram that we call an 'instability strip' or an 'instability region'. When the star is in this area of the diagram it will become a variable star, one that varies in brightness over time.“ • “Mira stars are red giants (which began as low mass stars), with a temperature less than ...
16 Hubble s Law and Dark Matter
... Galaxy Collisions The separation between galaxies is usually not large compared to the size of the galaxies themselves, and galactic collisions are frequent. The “cartwheel” galaxy on the left appears to be the result of a head-on collision with another ...
... Galaxy Collisions The separation between galaxies is usually not large compared to the size of the galaxies themselves, and galactic collisions are frequent. The “cartwheel” galaxy on the left appears to be the result of a head-on collision with another ...
Chapter 1-3
... Galaxy. Together they provide evidence for the chemical evolution of the Galaxy: the abundance of heavy elements (Z) apparently increases with time. This is the result of chemical enrichment by subsequent stellar generations. The study of chemical evolution has led to the hypothesis of a ‘Population ...
... Galaxy. Together they provide evidence for the chemical evolution of the Galaxy: the abundance of heavy elements (Z) apparently increases with time. This is the result of chemical enrichment by subsequent stellar generations. The study of chemical evolution has led to the hypothesis of a ‘Population ...
Neil F. Comins - Kuwait Life Sciences Company
... PREFACE away. View 2,500,000 stars along with more than 170 deep-space objects such as galaxies, star clusters, and nebulae. Travel 15,000 years in time, check out the view from the International Space Station, and see planets up close from any one of their moons. Included are stunning OpenGL graph ...
... PREFACE away. View 2,500,000 stars along with more than 170 deep-space objects such as galaxies, star clusters, and nebulae. Travel 15,000 years in time, check out the view from the International Space Station, and see planets up close from any one of their moons. Included are stunning OpenGL graph ...
The asymmetric nuclear region of M83 and its off
... M83 is a nearby (D=4.5 Mpc) barred spiral hosting a nuclear starburst. Our near infrared integral field spectroscopic data show the complexity of the inner 330 × 330 pc. The nuclear region reveals a pronounced asymmetry, with the optical peak displaced eastwards from the centre of fainter isophotes, ...
... M83 is a nearby (D=4.5 Mpc) barred spiral hosting a nuclear starburst. Our near infrared integral field spectroscopic data show the complexity of the inner 330 × 330 pc. The nuclear region reveals a pronounced asymmetry, with the optical peak displaced eastwards from the centre of fainter isophotes, ...
14. The Milky Way Galaxy: A Spiral in Space
... 14.3 Galactic Structure • The Galactic halo and globular clusters formed very early; the halo is essentially spherical. All the stars in the halo are very old, and there is no gas and dust. • The Galactic disk is where the youngest stars are, as well as star formation regions—emission nebulae, larg ...
... 14.3 Galactic Structure • The Galactic halo and globular clusters formed very early; the halo is essentially spherical. All the stars in the halo are very old, and there is no gas and dust. • The Galactic disk is where the youngest stars are, as well as star formation regions—emission nebulae, larg ...
Giant molecular clouds in the dwarf galaxy NGC 1569
... dwarf starburst galaxy NGC 1569 with the IRAM interferometer on Plateau de Bure. We find the CO emission is not spatially associated with the two super star clusters in the galaxy, but rather is found in the vicinity of an HII region. With the resolution of our data, we can resolve the CO emission i ...
... dwarf starburst galaxy NGC 1569 with the IRAM interferometer on Plateau de Bure. We find the CO emission is not spatially associated with the two super star clusters in the galaxy, but rather is found in the vicinity of an HII region. With the resolution of our data, we can resolve the CO emission i ...
Geoscience Astronomy Formative on Stellar Evolution and
... d. stars with two magnetic poles c. the time it takes light to travel one parsec the distance from Earth to the Sun ...
... d. stars with two magnetic poles c. the time it takes light to travel one parsec the distance from Earth to the Sun ...
AAVSO: Mu Cephei, October 2002 Variable Star Of The Month
... Here we ought to observe, that it is not easy to prove a star to be newly come; for though it should not be contained in any catalogue whatsoever, yet the argument for its former non-appearance, which is taken from its not having been observed, is only so far to be regarded as it can be made probabl ...
... Here we ought to observe, that it is not easy to prove a star to be newly come; for though it should not be contained in any catalogue whatsoever, yet the argument for its former non-appearance, which is taken from its not having been observed, is only so far to be regarded as it can be made probabl ...
![Module 4.1 - The Scale of the Universe [slide 1] We now turn to](http://s1.studyres.com/store/data/002846843_1-9e0ec9d1a2abbbab3c0d406694bfc4e2-300x300.png)
Module 4.1 - The Scale of the Universe [slide 1] We now turn to
... Since all of them were roughly the same distance, apparent magnitude would correlate with period and then they understood that comparing that with nearby Cepheids they can find out how far the Magellanic Couds are. Cepheids are important because they are bright and so we can see them far away, we c ...
... Since all of them were roughly the same distance, apparent magnitude would correlate with period and then they understood that comparing that with nearby Cepheids they can find out how far the Magellanic Couds are. Cepheids are important because they are bright and so we can see them far away, we c ...
(Science 2012) Gal-Yam
... from theoretical models of massive cores exploding via the pair-instability process. A lower ejecta mass (M = 43 M⊙) has been proposed (18). In any case, there is no doubt that these explosions are produced by extremely massive stars, with the most massive exploding heavy-element cores known to date ...
... from theoretical models of massive cores exploding via the pair-instability process. A lower ejecta mass (M = 43 M⊙) has been proposed (18). In any case, there is no doubt that these explosions are produced by extremely massive stars, with the most massive exploding heavy-element cores known to date ...
Astro Physics Notes and Study Guide 2015-17
... energy required to bump its electrons into higher orbitals because it has none. Cold hydrogen can absorb energy. Therefore, even if the emission spectrum has a dark line at hydrogen it could mean that there is hydrogen; it was just to “hot” to absorb energy. In this way, a VERY carful analysis of th ...
... energy required to bump its electrons into higher orbitals because it has none. Cold hydrogen can absorb energy. Therefore, even if the emission spectrum has a dark line at hydrogen it could mean that there is hydrogen; it was just to “hot” to absorb energy. In this way, a VERY carful analysis of th ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.