NASA`s Spitzer Images Out-of-This
... http://www.jpl.nasa.gov/multimedia/slideshows/spitzer-200605/slide4.cfm Splendid Splinter Seite 3 von 7 ...
... http://www.jpl.nasa.gov/multimedia/slideshows/spitzer-200605/slide4.cfm Splendid Splinter Seite 3 von 7 ...
Neutron stars and quark stars - Goethe
... Signals for Strange Stars? similar masses and radii, cooling, surface (crust), . . . but look for • extremely small mass, small radius stars (includes strangelets!) • strange dwarfs: small and light white dwarfs with a strange star core (Glendenning, Kettner, Weber, 1995) • super-Eddington luminosi ...
... Signals for Strange Stars? similar masses and radii, cooling, surface (crust), . . . but look for • extremely small mass, small radius stars (includes strangelets!) • strange dwarfs: small and light white dwarfs with a strange star core (Glendenning, Kettner, Weber, 1995) • super-Eddington luminosi ...
Chapter 31 - The Galaxy & Universe
... 3. All galaxies are moving away from all other galaxies (not just ...
... 3. All galaxies are moving away from all other galaxies (not just ...
Turbulent Flow-Driven Molecular Cloud Formation: A Solution to the
... The great majority of the stars have ages near 1 Myr; approximately half are younger than this, while only a few stars have ages greater than 3 Myr (see Fig 1 b). The group of stars near the 100 Myr isochrone (i.e., near the zero-age main sequence) were discovered through early Einstein X-ray survey ...
... The great majority of the stars have ages near 1 Myr; approximately half are younger than this, while only a few stars have ages greater than 3 Myr (see Fig 1 b). The group of stars near the 100 Myr isochrone (i.e., near the zero-age main sequence) were discovered through early Einstein X-ray survey ...
Chapter 12: Measuring the Properties of Stars
... this atom to absorb a photon, that photon must be of the right energy to move the electron from level 2 to higher levels. These photons are part of the Balmer series and are in the visible range. 3. A complete analysis would require examining a number of lines of several different chemical elements. ...
... this atom to absorb a photon, that photon must be of the right energy to move the electron from level 2 to higher levels. These photons are part of the Balmer series and are in the visible range. 3. A complete analysis would require examining a number of lines of several different chemical elements. ...
SXDS Highlights : Subaru / FOCAS Spectroscopy
... HST/NICMOS H-band Observations are not sufficient ! H-band observation only covers up to 4000A in the rest-frame, and star-forming regions can dominate the morphology. HST/NICMOS sample is limited to a small number of objects in Hubble Deep Field and does not have bright (~Mv*) galaxies at z~3. The ...
... HST/NICMOS H-band Observations are not sufficient ! H-band observation only covers up to 4000A in the rest-frame, and star-forming regions can dominate the morphology. HST/NICMOS sample is limited to a small number of objects in Hubble Deep Field and does not have bright (~Mv*) galaxies at z~3. The ...
Westerlund 1 : A Super-Star Cluster within the Milky Way
... identified in the Milky Way. Wd1 hosts a rich population of OB supergiants, Wolf-Rayet stars, Luminous Blue Variables, Yellow Hypergiants and Red Supergiants, from which we infer an age of 3-5Myr. For an adopted Kroupa IMF we derive a mass of 105 M and radius of 0.3pc for an estimated distance of 2 ...
... identified in the Milky Way. Wd1 hosts a rich population of OB supergiants, Wolf-Rayet stars, Luminous Blue Variables, Yellow Hypergiants and Red Supergiants, from which we infer an age of 3-5Myr. For an adopted Kroupa IMF we derive a mass of 105 M and radius of 0.3pc for an estimated distance of 2 ...
fred`s 2017 astronomy challenge
... see without equipment of some kind. Also, as it is moving over the sky, and even going behind the Sun and out of sight for a while at the beginning of the year, it’s trajectory ...
... see without equipment of some kind. Also, as it is moving over the sky, and even going behind the Sun and out of sight for a while at the beginning of the year, it’s trajectory ...
Lecture 7
... Core: R~ 0.01Rsun, ~1015 g/cm3, M~1.4Msun Eventually neutron degeneracy pressure opposes collapse (can be exceeded by ~50%), core-bounce – contraction of core heats outer layers which burn explosively, star literally explodes as a Type II Supernova leaving dense core of neutrons (R~5km) – a neutron ...
... Core: R~ 0.01Rsun, ~1015 g/cm3, M~1.4Msun Eventually neutron degeneracy pressure opposes collapse (can be exceeded by ~50%), core-bounce – contraction of core heats outer layers which burn explosively, star literally explodes as a Type II Supernova leaving dense core of neutrons (R~5km) – a neutron ...
The Sun and the Stars
... Core: R~ 0.01Rsun, ~1015 g/cm3, M~1.4Msun Eventually neutron degeneracy pressure opposes collapse (can be exceeded by ~50%), core-bounce – contraction of core heats outer layers which burn explosively, star literally explodes as a Type II Supernova leaving dense core of neutrons (R~5km) – a neutron ...
... Core: R~ 0.01Rsun, ~1015 g/cm3, M~1.4Msun Eventually neutron degeneracy pressure opposes collapse (can be exceeded by ~50%), core-bounce – contraction of core heats outer layers which burn explosively, star literally explodes as a Type II Supernova leaving dense core of neutrons (R~5km) – a neutron ...
Modified True/False - Indicate whether the statement is true or false
... HS-ESS1-1 When hydrogen nuclei fuse, they produce helium. HS-ESS1-1 A cloud of dust and gas in which a star forms is called a nebula. HS-ESS1-1 As white dwarfs cool, they often explode as supernovas. HS-ESS1-1 Combining of lightweight nuclei into heavier nuclei, such as four hydrogen nuclei combinin ...
... HS-ESS1-1 When hydrogen nuclei fuse, they produce helium. HS-ESS1-1 A cloud of dust and gas in which a star forms is called a nebula. HS-ESS1-1 As white dwarfs cool, they often explode as supernovas. HS-ESS1-1 Combining of lightweight nuclei into heavier nuclei, such as four hydrogen nuclei combinin ...
Part 1: If a 10000 K blackbody has a wavelength of peak emission at
... temperature of 10000 degrees (K). Both stars have the same radius. What is the luminosity ratio of Star B to Star A? This is all covered in Module 2 Lecture A and it was done in class on more than one occasion. It is also directly in the self study questions. It is fundamental to blackbody radiation ...
... temperature of 10000 degrees (K). Both stars have the same radius. What is the luminosity ratio of Star B to Star A? This is all covered in Module 2 Lecture A and it was done in class on more than one occasion. It is also directly in the self study questions. It is fundamental to blackbody radiation ...
has occurred over the past 14 billion years COSMIC DOWNSIZING
... redshift. Because of the universe’s expansion, the light from distant sources has been stretched, shifting its wavelength toward the red end of the spectrum. The more the light is shifted to the red, the farther away the source is and thus the older it is. For example, a redshift of one means that t ...
... redshift. Because of the universe’s expansion, the light from distant sources has been stretched, shifting its wavelength toward the red end of the spectrum. The more the light is shifted to the red, the farther away the source is and thus the older it is. For example, a redshift of one means that t ...
Goal: To understand the structure and makeup of our own Milky Way
... • It turns out that most of our galaxy is DARK MATTER. • If you look at stars and gas and dust the mass of our galaxy is about 100 billion solar masses. • However, the gravitational mass (M = V2* R / G) is 1 trillion solar masses! • 80-90% of our galaxy is mass we cannot see! ...
... • It turns out that most of our galaxy is DARK MATTER. • If you look at stars and gas and dust the mass of our galaxy is about 100 billion solar masses. • However, the gravitational mass (M = V2* R / G) is 1 trillion solar masses! • 80-90% of our galaxy is mass we cannot see! ...
Chapter 15: The Deaths of Massive Stars
... energy lost as the object slows down with the amount of energy emitted by the nebula. 5. The Crab pulsar spins so rapidly because it formed relatively recently. Over time it will lose rotational energy, slow down, and emit less energy. 6. The final fate of a pulsar depends on its neighborhood. A pul ...
... energy lost as the object slows down with the amount of energy emitted by the nebula. 5. The Crab pulsar spins so rapidly because it formed relatively recently. Over time it will lose rotational energy, slow down, and emit less energy. 6. The final fate of a pulsar depends on its neighborhood. A pul ...
Complete the “Assess Your Understanding” including
... Eventually, the outer _______________________________________________ to form a ___________________________________________ called a __________ _________________. The blue-white ____________ that is left behind _________ and becomes a _____________________. A white dwarf is about the size of Earth b ...
... Eventually, the outer _______________________________________________ to form a ___________________________________________ called a __________ _________________. The blue-white ____________ that is left behind _________ and becomes a _____________________. A white dwarf is about the size of Earth b ...
plagiarism - Homeschool
... Stars, rocks and people all emit light, and and people included. The temperature of which wavelength of light will be most the star, rock or person determines which strongly radiated depends on the wavelength of light will be most strongly temperature of the star, rock or person. For radiated. In th ...
... Stars, rocks and people all emit light, and and people included. The temperature of which wavelength of light will be most the star, rock or person determines which strongly radiated depends on the wavelength of light will be most strongly temperature of the star, rock or person. For radiated. In th ...
The Milky Way galaxy Contents Summary
... billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Universe is contributed by galaxies that lie just below the top of the scale. The Sun lies in just such a g ...
... billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Universe is contributed by galaxies that lie just below the top of the scale. The Sun lies in just such a g ...
Quantum effects in astrophysics
... collisions can trigger the transitions. The distribution of hydrogen in the Galaxy was first mapped by 1420 MHz observations. This was possible because radio waves are not absorbed by intervening gas and dust that bocks visible light. It is interesting that we now have very good maps of the distribu ...
... collisions can trigger the transitions. The distribution of hydrogen in the Galaxy was first mapped by 1420 MHz observations. This was possible because radio waves are not absorbed by intervening gas and dust that bocks visible light. It is interesting that we now have very good maps of the distribu ...
Determining the Sizes & Distances of Stars Using the H
... cores, but after awhile they evolve and begin to die. How long they live and what they evolve to become when they die depends on their mass. In fact, the mass of a star also determines its most important properties: its luminosity, temperature and radius. A star's luminosity, which is how much energ ...
... cores, but after awhile they evolve and begin to die. How long they live and what they evolve to become when they die depends on their mass. In fact, the mass of a star also determines its most important properties: its luminosity, temperature and radius. A star's luminosity, which is how much energ ...
Ercolano et al. 2009 - Institute of Astronomy
... 2) High mass star formation – Radiation Pressure on dust grains 3) High mass star formation – Ionisation Feedback & Triggered star formation ...
... 2) High mass star formation – Radiation Pressure on dust grains 3) High mass star formation – Ionisation Feedback & Triggered star formation ...
10 - Keele Astrophysics Group
... Early in the 19th century, the German physicist Joseph von Fraunhofer observed the solar spectrum and realised that there was a clear pattern of absorption lines superimposed on the continuum. By the end of that century, astronomers were able to examine the spectra of stars in large numbers and real ...
... Early in the 19th century, the German physicist Joseph von Fraunhofer observed the solar spectrum and realised that there was a clear pattern of absorption lines superimposed on the continuum. By the end of that century, astronomers were able to examine the spectra of stars in large numbers and real ...
FORMATION OF LATE-TYPE SPIRAL GALAXIES: GAS RETURN
... matter halos through a combination of hierarchical merging and gas accretion along cold streams. Cosmological simulations thus predict that galaxies rapidly grow their bulge through mergers and instabilities and end up with most of their mass in the bulge and an angular momentum much below the obser ...
... matter halos through a combination of hierarchical merging and gas accretion along cold streams. Cosmological simulations thus predict that galaxies rapidly grow their bulge through mergers and instabilities and end up with most of their mass in the bulge and an angular momentum much below the obser ...
Chapter 2 Observing the Electromagnetic Spectrum
... The High Energy Astrophysical Observatory-2 (HEAO-2), later named Einstein, was launched into low Earth orbit on November 13th, 1978 and operated until April, 1981. It was the first X-ray mission to use focusing optics with imaging detectors and produce angular resolution of a few arc seconds3 ( ′′ ...
... The High Energy Astrophysical Observatory-2 (HEAO-2), later named Einstein, was launched into low Earth orbit on November 13th, 1978 and operated until April, 1981. It was the first X-ray mission to use focusing optics with imaging detectors and produce angular resolution of a few arc seconds3 ( ′′ ...
Origin of the Solar System
... proceeds, the gravitational energy released will be partitioned equally between radiation and heating. If this continues long enough, the radiative flux from the protostar will become important in shaping its surroundings, e.g., by heating the surrounding dust. The second is that the continued decre ...
... proceeds, the gravitational energy released will be partitioned equally between radiation and heating. If this continues long enough, the radiative flux from the protostar will become important in shaping its surroundings, e.g., by heating the surrounding dust. The second is that the continued decre ...
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.