Chapter 10 Cycles and Patterns in Space D64 Lesson Preview
... star is a ball of hot gases that gives off light and other forms of energy. Stars come in different sizes. The smallest stars are only about 20 km (about 12 mi) across. White dwarf stars are about the size of Earth. Supergiant stars can be more than 500 million km (about 300 million mi) wide. That i ...
... star is a ball of hot gases that gives off light and other forms of energy. Stars come in different sizes. The smallest stars are only about 20 km (about 12 mi) across. White dwarf stars are about the size of Earth. Supergiant stars can be more than 500 million km (about 300 million mi) wide. That i ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... of SOXS is composed by 7 XMM-Newton observations to which we have added 3 archive pointings. The maps below are the RGB mosaics of X-ray images of EPIC on board XMM-Newton and IR images of IRAC on board Spitzer. The upper crowded field is the archive Iota Ori observation, in which the bright O-type ...
... of SOXS is composed by 7 XMM-Newton observations to which we have added 3 archive pointings. The maps below are the RGB mosaics of X-ray images of EPIC on board XMM-Newton and IR images of IRAC on board Spitzer. The upper crowded field is the archive Iota Ori observation, in which the bright O-type ...
The Physics of Star Formation: Understanding the Youngest Protostars
... resolution and sensitivity to study them in the mid-IR regime. SOFIA will lack the sensitivity and spatial resolution required for these observations. Although ISO performed a pioneering observation of the 63 m [OI] feature in an accretion shock for the most luminous Class 0 source IRAS 16293{2422 ...
... resolution and sensitivity to study them in the mid-IR regime. SOFIA will lack the sensitivity and spatial resolution required for these observations. Although ISO performed a pioneering observation of the 63 m [OI] feature in an accretion shock for the most luminous Class 0 source IRAS 16293{2422 ...
Dynamics of elliptical galaxies
... of the total light in the galaxy. Measure three apparently independent properties; • The effective radius Re • The central velocity dispersion s • The surface brightness at the effective radius Ie=I(Re) Plot these quantities in three dimensions - find that the points all lie close to a single plane! ...
... of the total light in the galaxy. Measure three apparently independent properties; • The effective radius Re • The central velocity dispersion s • The surface brightness at the effective radius Ie=I(Re) Plot these quantities in three dimensions - find that the points all lie close to a single plane! ...
Stargazing For Beginners: A Binocular Tour of the Southern Night Sky
... This course introduces you to the bright stars and major constellations visible from the Southern Hemisphere, along with dozens of deep-sky sights of interest within each constellation, such as galaxies, binary stars, nebulae, and star clusters. It assumes you are equipped with nothing more than a s ...
... This course introduces you to the bright stars and major constellations visible from the Southern Hemisphere, along with dozens of deep-sky sights of interest within each constellation, such as galaxies, binary stars, nebulae, and star clusters. It assumes you are equipped with nothing more than a s ...
PARALLAX – IT`S SIMPLE! Abstract
... The first stellar parallax was measured by German astronomer F.W. Bessel in 1838. The parallax angle of star Cygnus 61 was very small, some tenths of arcsecond and hard to measure. Even for the nearest star, Alpha Centauri the annual parallax is less than 1 arcsecond (less than 1/3600 of one arc deg ...
... The first stellar parallax was measured by German astronomer F.W. Bessel in 1838. The parallax angle of star Cygnus 61 was very small, some tenths of arcsecond and hard to measure. Even for the nearest star, Alpha Centauri the annual parallax is less than 1 arcsecond (less than 1/3600 of one arc deg ...
Lecture Topics 1023
... These are the headings of the paragraphs into which ASTR 1023 lectures are divided. Use them to check your notes for completeness, and to see how the course is organized. It is also a good idea to cross-check these topics with your reading assignments, because some topics are not in the textbook. Le ...
... These are the headings of the paragraphs into which ASTR 1023 lectures are divided. Use them to check your notes for completeness, and to see how the course is organized. It is also a good idea to cross-check these topics with your reading assignments, because some topics are not in the textbook. Le ...
Larger, high-res file, best for printing
... apparently unremarkable Cas A supernova event. Perhaps the simplest explanation is that the supernova reached its peak luminosity when Cassiopeia was high in the daylight sky. Or this particular supernova may have had such a low intrinsic luminosity that it was simply too dim for most 17th-century a ...
... apparently unremarkable Cas A supernova event. Perhaps the simplest explanation is that the supernova reached its peak luminosity when Cassiopeia was high in the daylight sky. Or this particular supernova may have had such a low intrinsic luminosity that it was simply too dim for most 17th-century a ...
Mass loss of massive stars near the Eddington luminosity by core
... Eddington luminosity (e.g., Gal-Yam & Leonard 2009; Smith et al. 2011). The high luminosity is often related to LBVs, which are known to experience the enhanced mass loss required to explain the observational properties of Type IIn SNe (e.g., Smith 2006). However, LBVs are not SN progenitors in stan ...
... Eddington luminosity (e.g., Gal-Yam & Leonard 2009; Smith et al. 2011). The high luminosity is often related to LBVs, which are known to experience the enhanced mass loss required to explain the observational properties of Type IIn SNe (e.g., Smith 2006). However, LBVs are not SN progenitors in stan ...
in search of antimatter in the universe
... ellipse. One such galaxy is Centaurus A, which is the closest galaxy to us with an AGN jet, at 3.7 Mega parsecs (1 parsec is 3.1x1016 m). This means its jet can be studied in greater detail than is possible in more remote sources. (Figure 5). This has allowed ‘knots’ in the jet to be resolved in x-r ...
... ellipse. One such galaxy is Centaurus A, which is the closest galaxy to us with an AGN jet, at 3.7 Mega parsecs (1 parsec is 3.1x1016 m). This means its jet can be studied in greater detail than is possible in more remote sources. (Figure 5). This has allowed ‘knots’ in the jet to be resolved in x-r ...
Autumn 2016 Midterm Review - Autumn 2015 Questions
... 22. We have learned that nuclear fusion - the proton-proton chain - is occurring in the deepest part, the very core, of the Sun. What does this have to do with us? a. The gamma rays being produced provide the radiative support for the Sun. b. Eventually that energy gets transferred through the Sun a ...
... 22. We have learned that nuclear fusion - the proton-proton chain - is occurring in the deepest part, the very core, of the Sun. What does this have to do with us? a. The gamma rays being produced provide the radiative support for the Sun. b. Eventually that energy gets transferred through the Sun a ...
The fate of black hole singularities and the parameters of the
... small change in any parameter leading to an increase in the number of black holes produced in the universe. iii) Given reasonable and widely believed assumptions about star formation processes in spiral galaxies there are clear arguments that at least seven distinct small changes in the parameters t ...
... small change in any parameter leading to an increase in the number of black holes produced in the universe. iii) Given reasonable and widely believed assumptions about star formation processes in spiral galaxies there are clear arguments that at least seven distinct small changes in the parameters t ...
Enhanced lithium depletion in Sun-like stars with orbiting planets.
... 451 stars in the HARPS high precision (better than 1 m/s) radial velocity exoplanet survey11 spanning the effective temperature range between 4900 and 6500 K. These are unevolved, slowly rotating non-active stars from a CORALIE catalogue11. These stars have been monitored with high precision spectro ...
... 451 stars in the HARPS high precision (better than 1 m/s) radial velocity exoplanet survey11 spanning the effective temperature range between 4900 and 6500 K. These are unevolved, slowly rotating non-active stars from a CORALIE catalogue11. These stars have been monitored with high precision spectro ...
arXiv:1502.04693v1 [gr
... important. We investigate in detail the possibility of delensing the CMB with the cosmic infrared background (CIB), emission from dusty star-forming galaxies that is an excellent tracer of the CMB lensing signal, in order to improve constraints on the tensor-to-scalar ratio r. We find that the maps ...
... important. We investigate in detail the possibility of delensing the CMB with the cosmic infrared background (CIB), emission from dusty star-forming galaxies that is an excellent tracer of the CMB lensing signal, in order to improve constraints on the tensor-to-scalar ratio r. We find that the maps ...
Planets orbiting stars more massive than the Sun
... must have detected all transiting giant planets with short orbital periods in these fields. To determine the frequency of close-in planets and BDs, all we have to do is to find out whether the transits are false-positives (FPs), eclipsing binaries, or not. After excluding binaries, and all types of ...
... must have detected all transiting giant planets with short orbital periods in these fields. To determine the frequency of close-in planets and BDs, all we have to do is to find out whether the transits are false-positives (FPs), eclipsing binaries, or not. After excluding binaries, and all types of ...
Galaxies - Stockton University
... Galaxies on the other hand have sizes ranging from 1 to 100 Kpc, but are separated by of order 1 to 10 Mpc from their neighbors, only a factor of 100 to 1000. This means that almost all galaxies have probably had direct interactions, collisions and mergers with others during their lives. For an indi ...
... Galaxies on the other hand have sizes ranging from 1 to 100 Kpc, but are separated by of order 1 to 10 Mpc from their neighbors, only a factor of 100 to 1000. This means that almost all galaxies have probably had direct interactions, collisions and mergers with others during their lives. For an indi ...
Video Lesson Information Astronomy: Observations & Theories Astronomy 1
... constellations, and brought the aspects of the sky into their buildings and structures, such as those of Chaco Canyon in the southwestern United States. Lesson 3 - Celestial Cycles This video lesson explains the motion of Earth around the sun and its yearly cycle. Astronomers explain the unique orbi ...
... constellations, and brought the aspects of the sky into their buildings and structures, such as those of Chaco Canyon in the southwestern United States. Lesson 3 - Celestial Cycles This video lesson explains the motion of Earth around the sun and its yearly cycle. Astronomers explain the unique orbi ...
The Age and Progenitor Mass of Sirius B
... The Sirius system is the fifth or sixth nearest stellar system to the Sun1 , and certainly is one of the best studied binary systems including a white dwarf component. One does not want to employ a white dwarf in a binary close enough that interactions might have affected the mass loss phases in the ...
... The Sirius system is the fifth or sixth nearest stellar system to the Sun1 , and certainly is one of the best studied binary systems including a white dwarf component. One does not want to employ a white dwarf in a binary close enough that interactions might have affected the mass loss phases in the ...
USRA - MSU Solar Physics
... Without compromising much collecting power, its medium size allows for fast acquisition times compared to large telescopes such as Hawaii’s Keck Observatory. WIRO has been undergoing renovation similar to that of RBO with upgraded instruments and facility improvements. Recent additions are WIRO’s th ...
... Without compromising much collecting power, its medium size allows for fast acquisition times compared to large telescopes such as Hawaii’s Keck Observatory. WIRO has been undergoing renovation similar to that of RBO with upgraded instruments and facility improvements. Recent additions are WIRO’s th ...
Ursa Minor
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.