FEEDBACK IN THE LOCAL UNIVERSE: The
... radio source has returned upwards of 1061 erg to regions of the cluster that extend even beyond the cooling radius. Note the strong spatial anti-correlation of the radio source (in pink) with the X-ray cavities (in blue). Such correspondence is typical of cool core clusters with cavities and extende ...
... radio source has returned upwards of 1061 erg to regions of the cluster that extend even beyond the cooling radius. Note the strong spatial anti-correlation of the radio source (in pink) with the X-ray cavities (in blue). Such correspondence is typical of cool core clusters with cavities and extende ...
Document
... changes. From an observed line profile, one can construct an image of the surface of the star. This technique has been applied to many different types of stars. ...
... changes. From an observed line profile, one can construct an image of the surface of the star. This technique has been applied to many different types of stars. ...
The Northern Winter Constellations - Science
... The Constellations of the Winter Sky If you live in the northern latitudes and you scan the sky from the southern horizon to the region overhead, you should be able to see the following constellations on a clear winter night: Orion the Hunter, Canis Major the Great Dog, Canis Minor the Little Dog, T ...
... The Constellations of the Winter Sky If you live in the northern latitudes and you scan the sky from the southern horizon to the region overhead, you should be able to see the following constellations on a clear winter night: Orion the Hunter, Canis Major the Great Dog, Canis Minor the Little Dog, T ...
Characteristics of Main Sequence Stars
... masses, due to the contribution of radiation pressure in the central core. (This helps support the star, and decreases the central temperature slightly.) The relation also flattens significantly at the very faint end of the luminosity function. This is due to the increasing important of convection f ...
... masses, due to the contribution of radiation pressure in the central core. (This helps support the star, and decreases the central temperature slightly.) The relation also flattens significantly at the very faint end of the luminosity function. This is due to the increasing important of convection f ...
the rest of the univ..
... resonance with Neptune (as does Pluto). Color measurements of some of the brightest have shown that they are unusually red. Some astronomers believe that Pluto (and Charon) ought to be classified as part of this class. It is estimated that there are at least 35,000 Kuiper Belt objects greater than ...
... resonance with Neptune (as does Pluto). Color measurements of some of the brightest have shown that they are unusually red. Some astronomers believe that Pluto (and Charon) ought to be classified as part of this class. It is estimated that there are at least 35,000 Kuiper Belt objects greater than ...
Lecture21
... • The model is a strong dipole magnetic field, inclined to the rotation axis. • The time-varying electric and magnetic fields form an EM wave that carries energy away from the star as magnetic dipole radiation. • Electrons or ions are propelled from the strong gravitational field. As they spiral aro ...
... • The model is a strong dipole magnetic field, inclined to the rotation axis. • The time-varying electric and magnetic fields form an EM wave that carries energy away from the star as magnetic dipole radiation. • Electrons or ions are propelled from the strong gravitational field. As they spiral aro ...
Properties of Stars: The H
... well understood and we will get back to these next section when we talk about the energy source for stars. • Note that all the extra-solar planets that are being discovered at a rate of about 10 per year are detected by the Doppler shift of the stars around which they orbit. These are essentially si ...
... well understood and we will get back to these next section when we talk about the energy source for stars. • Note that all the extra-solar planets that are being discovered at a rate of about 10 per year are detected by the Doppler shift of the stars around which they orbit. These are essentially si ...
Discovery of Warm and Dense Molecular Gas Surrounding the Ring
... This significant result encourages the search for molecular gas in the environs of evolved massive stars which have not yet become Wolf-Rayet. Of those, the luminous blue variable ( LBV ) stars are probably the best candidates, due to the ‘‘instantaneous’’ effect of their strong winds and spectacula ...
... This significant result encourages the search for molecular gas in the environs of evolved massive stars which have not yet become Wolf-Rayet. Of those, the luminous blue variable ( LBV ) stars are probably the best candidates, due to the ‘‘instantaneous’’ effect of their strong winds and spectacula ...
Chap. 02
... In practice, “zero-age” means that the star has changed so little in radius, effective temperature and luminosity – Means a few thousand years for a massive star – Means 10 million years for the Sun – Means 1 billion years for the least massive stars ...
... In practice, “zero-age” means that the star has changed so little in radius, effective temperature and luminosity – Means a few thousand years for a massive star – Means 10 million years for the Sun – Means 1 billion years for the least massive stars ...
So, what`s the problem for high
... far-IR (50-200m), dust emission gives virtually total luminosity (power in watts). In millimeter and submillimeter wavelengths, dust emission can be used to measure the mass of a molecular cloud, and its star forming cores. ...
... far-IR (50-200m), dust emission gives virtually total luminosity (power in watts). In millimeter and submillimeter wavelengths, dust emission can be used to measure the mass of a molecular cloud, and its star forming cores. ...
CHAPTER 14
... 3. The material in the shell glows because UV radiation from the central hot star causes it to fluoresce. 4. Pulsations in the core of the red giant and/or stellar winds emitted from the dying star (and which occur in definite stages) are thought to cause planetary nebulae. 5. Not all planetary nebu ...
... 3. The material in the shell glows because UV radiation from the central hot star causes it to fluoresce. 4. Pulsations in the core of the red giant and/or stellar winds emitted from the dying star (and which occur in definite stages) are thought to cause planetary nebulae. 5. Not all planetary nebu ...
Exam 03
... D) Red. The reflection nebula is hot and glows red because of the strong H-α emission line. E) Blue. A cool reflection nebula reflects and scatters the blue light that strikes it. 53. An emission nebula will typically appear A) White. A nebula is a cloud of water vapor, so it appears white or maybe ...
... D) Red. The reflection nebula is hot and glows red because of the strong H-α emission line. E) Blue. A cool reflection nebula reflects and scatters the blue light that strikes it. 53. An emission nebula will typically appear A) White. A nebula is a cloud of water vapor, so it appears white or maybe ...
here - ESA Science
... concept of the celestial sphere on which stars have been grouped into constellations since ancient times. What is difficult to imagine when looking at the night sky is the immense depth of the sky; we do not get a 3dimensional view. From Earth each and every star seen with the unaided eye belongs to ...
... concept of the celestial sphere on which stars have been grouped into constellations since ancient times. What is difficult to imagine when looking at the night sky is the immense depth of the sky; we do not get a 3dimensional view. From Earth each and every star seen with the unaided eye belongs to ...
Rosolowsky
... • GMCs appear to unify the star formation process across a variety of environments. • Suggests important factor in SF is the conversion of gas into GMCs. • Conversion efficiency (and process?) varies across environments. ...
... • GMCs appear to unify the star formation process across a variety of environments. • Suggests important factor in SF is the conversion of gas into GMCs. • Conversion efficiency (and process?) varies across environments. ...
Lecture 24, The local group
... to look intermediate between globular clusters and dwarf galaxies ...
... to look intermediate between globular clusters and dwarf galaxies ...
Virtual HR Diagram Lab
... b. Now manipulate the temperature and luminosity sliders and note the corresponding change in the active location. Fill in the table below. ...
... b. Now manipulate the temperature and luminosity sliders and note the corresponding change in the active location. Fill in the table below. ...
High Mass Stars
... – From H-R diagram its luminosity is 100000 times greater than the Sun’s. – It therefore burns fuel (uses it’s mass) 100000 times faster than the Sun. – It has 25 times the mass of the Sun so its lifetime will be 25/100000 = 0.00025 times than the Sun’s lifetime = 2.5 million years. ...
... – From H-R diagram its luminosity is 100000 times greater than the Sun’s. – It therefore burns fuel (uses it’s mass) 100000 times faster than the Sun. – It has 25 times the mass of the Sun so its lifetime will be 25/100000 = 0.00025 times than the Sun’s lifetime = 2.5 million years. ...
H-R Diagram
... After the supernova blast blows off the outer layers of the star, all that is left is the central core. The core now contains a mass between 1.4 and 3.0 times the sun's mass but condensed into a volume 10- to 20km across - roughly the size of a small town on Earth. The matter in a neutron star would ...
... After the supernova blast blows off the outer layers of the star, all that is left is the central core. The core now contains a mass between 1.4 and 3.0 times the sun's mass but condensed into a volume 10- to 20km across - roughly the size of a small town on Earth. The matter in a neutron star would ...
Phase Analysis of RV Tauri and Semi-regular Variables Abstract
... RV Tauri variable stars, related classes of pulsating variable stars. The ultimate objective for our research is to determine whether the stars stellar properties such as temperature, radius, and luminosity correlate with their pulsation cycles. In order to determine this, we need to closely examine ...
... RV Tauri variable stars, related classes of pulsating variable stars. The ultimate objective for our research is to determine whether the stars stellar properties such as temperature, radius, and luminosity correlate with their pulsation cycles. In order to determine this, we need to closely examine ...
What is a star?
... • Astronomers used telescopes see many stars that are too dim to see with the unaided eye. They added to the magnitude system. • Today, the brightest stars have a magnitude of about –2, and the faintest stars that we can see with a telescope have a magnitude of +30. • Dim stars have positive (larger ...
... • Astronomers used telescopes see many stars that are too dim to see with the unaided eye. They added to the magnitude system. • Today, the brightest stars have a magnitude of about –2, and the faintest stars that we can see with a telescope have a magnitude of +30. • Dim stars have positive (larger ...
CHAPTER 4 THE SPATIAL DISTRIBUTION OF GALAXIES 4.13
... Having looked at the properties of individual galaxies – both normal and active – in some detail, it is now appropriate to consider how these galaxies are distributed in space. Surveys of the region outside our own Milky Way show that there are galaxies all around us. Deep field images such as those ...
... Having looked at the properties of individual galaxies – both normal and active – in some detail, it is now appropriate to consider how these galaxies are distributed in space. Surveys of the region outside our own Milky Way show that there are galaxies all around us. Deep field images such as those ...
Observational properties of stars
... How do we track/follow the evolution of a star? Basic answer – it isn’t possible. Stars evolve very slowly so it is not possible to see significant changes in any stars during your life. There are occasional sporadic changes, like supernovae, but those are rare. Stars will take millions or billions ...
... How do we track/follow the evolution of a star? Basic answer – it isn’t possible. Stars evolve very slowly so it is not possible to see significant changes in any stars during your life. There are occasional sporadic changes, like supernovae, but those are rare. Stars will take millions or billions ...
Chapter 6 Stars
... Scientists have detected many star-size black holes with the Chandra X-ray Observatory. They have also detected huge black holes that are million or billions of times the sun’s mass. ...
... Scientists have detected many star-size black holes with the Chandra X-ray Observatory. They have also detected huge black holes that are million or billions of times the sun’s mass. ...
Astro 10: Introductory Astronomy
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
The Milky Way Galaxy
... the total amount of dark matter determines the fate of our Universe the Earth would be destroyed if it ever ran into a clump of cold dark matter dark matter is responsible for the formation of structure in our Universe our understanding of dark matter may reveal a new, undiscovered form of matter ...
... the total amount of dark matter determines the fate of our Universe the Earth would be destroyed if it ever ran into a clump of cold dark matter dark matter is responsible for the formation of structure in our Universe our understanding of dark matter may reveal a new, undiscovered form of matter ...
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.