Stellar Spectroscopy (GA 3.0) - National Optical Astronomy
... measure of the quantity of each color of light (or more specifically, the amount of each wavelength of light). It is a powerful tool in astronomy. In fact, most of what we know in astronomy is a result of spectroscopy: it can reveal the temperature, velocity and composition of an object as well as b ...
... measure of the quantity of each color of light (or more specifically, the amount of each wavelength of light). It is a powerful tool in astronomy. In fact, most of what we know in astronomy is a result of spectroscopy: it can reveal the temperature, velocity and composition of an object as well as b ...
HST Paα Survey of the Galactic Center – Seeking the Missing
... We find that many of the Paα-emitting stars are located outside of the three young massive star clusters. As we mentioned previously, they are evolved massive stars with ages of a few Myr. Studying their origin can help us understand the star formation mode within the GC. Two third of these field Pa ...
... We find that many of the Paα-emitting stars are located outside of the three young massive star clusters. As we mentioned previously, they are evolved massive stars with ages of a few Myr. Studying their origin can help us understand the star formation mode within the GC. Two third of these field Pa ...
Red Supergiants as Cosmic Abundance Probes
... by calibrating against either results from the direct method or from photoionisation models. The limitation of these strongline methods is that they have well-known systematic offsets from one another, particularly at high metallicity, where two different calibrations may give results ~ 0.8 dex apa ...
... by calibrating against either results from the direct method or from photoionisation models. The limitation of these strongline methods is that they have well-known systematic offsets from one another, particularly at high metallicity, where two different calibrations may give results ~ 0.8 dex apa ...
Astronomy Astrophysics
... 5200 km s−1 . Following Condon et al. (2002) we use the optical convention (v = cz) for all velocities. The atomic hydrogen (H) column densities are extremely high in the bridge region, reaching about 3 × 1021 cm−2 . Two H peaks, HE and HW , are also present in the outer parts of the common H e ...
... 5200 km s−1 . Following Condon et al. (2002) we use the optical convention (v = cz) for all velocities. The atomic hydrogen (H) column densities are extremely high in the bridge region, reaching about 3 × 1021 cm−2 . Two H peaks, HE and HW , are also present in the outer parts of the common H e ...
Chapter 19 Star Formation
... At stage 6, the core reaches 10 million K, and nuclear fusion begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. ...
... At stage 6, the core reaches 10 million K, and nuclear fusion begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. ...
1705 Star Charts
... Eta Carinae nebula, a luminous spot in the Milky Way to the right of Crux, is a glowing gas cloud about 8000 light years from us. The thin gas glows in the ultraviolet light of nearby hot young stars. The golden star in the cloud, visible in binoculars, is Eta [Greek ‘e’] Carinae. It is estimated to ...
... Eta Carinae nebula, a luminous spot in the Milky Way to the right of Crux, is a glowing gas cloud about 8000 light years from us. The thin gas glows in the ultraviolet light of nearby hot young stars. The golden star in the cloud, visible in binoculars, is Eta [Greek ‘e’] Carinae. It is estimated to ...
The GalMer database: galaxy mergers in the virtual observatory*
... of galaxy interactions for the modern picture of galaxy evolution. The GalMer project, developed in the framework of the French national HORIZON1 collaboration, has the ambitious goal of providing access for the astronomical community to the results of massive intermediate-resolution numerical simul ...
... of galaxy interactions for the modern picture of galaxy evolution. The GalMer project, developed in the framework of the French national HORIZON1 collaboration, has the ambitious goal of providing access for the astronomical community to the results of massive intermediate-resolution numerical simul ...
Broadening of spectral lines An individual atom/molecule making a
... !abundance of different elements, and on the excitation! !/ ionization state (described in part by the Boltzmann ! ...
... !abundance of different elements, and on the excitation! !/ ionization state (described in part by the Boltzmann ! ...
Active Galactic Nuclei at kiloparsec scales and their cosmological
... or entrainment of stellar wind gas from stars embedded within the jet flow (e.g., [66] and references therein). Another ingredient that has been proposed as causing the dichotomy is the magnetic field structure and intensity (e.g., [56] and references therein). The velocity profile of the jets -alon ...
... or entrainment of stellar wind gas from stars embedded within the jet flow (e.g., [66] and references therein). Another ingredient that has been proposed as causing the dichotomy is the magnetic field structure and intensity (e.g., [56] and references therein). The velocity profile of the jets -alon ...
charts_set_7
... Clusters are crucial for stellar evolution studies because: 1) All stars in a cluster formed about same time (so about same age) 2) All stars are at about the same distance 3) All stars have same chemical composition ...
... Clusters are crucial for stellar evolution studies because: 1) All stars in a cluster formed about same time (so about same age) 2) All stars are at about the same distance 3) All stars have same chemical composition ...
Gas disks to gas giants: Simulating the birth of planetary systems
... longer-timescale simulations usually model the time after the protostellar gas disk has dissipated, allowing the problem to be tackled with pure gravitational N-body methods. Recent work in this area has been successful at reproducing the observed exoplanet eccentricity distribution, the key requir ...
... longer-timescale simulations usually model the time after the protostellar gas disk has dissipated, allowing the problem to be tackled with pure gravitational N-body methods. Recent work in this area has been successful at reproducing the observed exoplanet eccentricity distribution, the key requir ...
Lecture 18, Gravitational Waves, Future Missions and
... Gravitational waves are often described as ripples in space-time. In general relativity, mass leads to a curvature of space-time. Gravity waves are produced by accelerating masses (if the motion is not perfectly symmetric). Gravity waves have not yet been detected, though we do have indirect evidenc ...
... Gravitational waves are often described as ripples in space-time. In general relativity, mass leads to a curvature of space-time. Gravity waves are produced by accelerating masses (if the motion is not perfectly symmetric). Gravity waves have not yet been detected, though we do have indirect evidenc ...
–1– Lectures 18 and 19 Optical Depth vs. Density Imaging a sphere
... We see that as a cloud collapses, the optical depth increases. At the same time, the Jeans length and mass will decrease. This leads to two competing effects. On one hand, the density increases, leading to higher optical depths. At the same time, Fred Hoyle in the 1950s predicted that as a cloud col ...
... We see that as a cloud collapses, the optical depth increases. At the same time, the Jeans length and mass will decrease. This leads to two competing effects. On one hand, the density increases, leading to higher optical depths. At the same time, Fred Hoyle in the 1950s predicted that as a cloud col ...
Galaxies - cloudfront.net
... Read this passage based on the text and answer the questions that follow. Types of Galaxies Galaxies are the biggest groups of stars in the universe. They can contain anywhere from a few million to many billions of stars. Galaxies are divided into three types according to shape: spiral, elliptical, ...
... Read this passage based on the text and answer the questions that follow. Types of Galaxies Galaxies are the biggest groups of stars in the universe. They can contain anywhere from a few million to many billions of stars. Galaxies are divided into three types according to shape: spiral, elliptical, ...
Gemini IFU Observations of Feedback from Radio
... cocoon, deposit mechanic energy into ISM/IGM - both in observations and simulations ...
... cocoon, deposit mechanic energy into ISM/IGM - both in observations and simulations ...
The Hubble Redshift Distance Relation
... must be located at the center of the Universe, but this is not the case. As we will discover in this lab, we are not in some preferred location in our Universe. In this lab we will also use the fact that galaxies appear to be moving away from us to infer an age for the Universe, based on the amount ...
... must be located at the center of the Universe, but this is not the case. As we will discover in this lab, we are not in some preferred location in our Universe. In this lab we will also use the fact that galaxies appear to be moving away from us to infer an age for the Universe, based on the amount ...
Star Formation 1 - Center for Astrostatistics
... So, the cloud of atoms starts gravitational collapse, gas heats up as density increase, and collapse stops when hydrostatic equilibriumis achieved; that is, when the inward pull of gravity and outward push of gas pressure are equal everywhere. The result is a sphere, hot & dense in the core, cooler ...
... So, the cloud of atoms starts gravitational collapse, gas heats up as density increase, and collapse stops when hydrostatic equilibriumis achieved; that is, when the inward pull of gravity and outward push of gas pressure are equal everywhere. The result is a sphere, hot & dense in the core, cooler ...
TAP 704- 8: The ladder of astronomical distances
... told that the Universe is only half as big as the astronomers present all thought, and therefore only half as old. The challenger was the French-American astronomer Gerard de Vaucouleurs; the leader of the challenged orthodoxy was Allan Sandage, who had inherited the mantle of the American astronome ...
... told that the Universe is only half as big as the astronomers present all thought, and therefore only half as old. The challenger was the French-American astronomer Gerard de Vaucouleurs; the leader of the challenged orthodoxy was Allan Sandage, who had inherited the mantle of the American astronome ...
Staring Back to Cosmic Dawn - UC-HiPACC
... At the present day, only a few galaxies lie between the peaks of the blue and red galaxies, in the so-called “green valley” (so named because green wavelengths are midway between red and blue in the spectrum). A blue galaxy that is vigorously forming stars will become green within a few hundred mill ...
... At the present day, only a few galaxies lie between the peaks of the blue and red galaxies, in the so-called “green valley” (so named because green wavelengths are midway between red and blue in the spectrum). A blue galaxy that is vigorously forming stars will become green within a few hundred mill ...
Heavy Metal from Ancient Superstars
... In the early galaxy, elements were forming very quickly from new star formation. The chemical mixture we see is different from the Solar System We find a much smaller amount of “metals” mixed in with the hydrogen and helium Heavy metals come only from supernovae – not from low mass stars ...
... In the early galaxy, elements were forming very quickly from new star formation. The chemical mixture we see is different from the Solar System We find a much smaller amount of “metals” mixed in with the hydrogen and helium Heavy metals come only from supernovae – not from low mass stars ...
The Main Features of the X
... molecular cloud falling into the plane of the Galaxy Cygnus Superbubble/Loop: nearby superbubble from the explosion of many Sne, 14 times the size (at 400 pc in diameter) of the Cynus Loop, a 20,000 year old SNR emitting thermal bremsstrahlung as soft x-rays. North Polar Spur (NPS)/Loop 1: The NPS i ...
... molecular cloud falling into the plane of the Galaxy Cygnus Superbubble/Loop: nearby superbubble from the explosion of many Sne, 14 times the size (at 400 pc in diameter) of the Cynus Loop, a 20,000 year old SNR emitting thermal bremsstrahlung as soft x-rays. North Polar Spur (NPS)/Loop 1: The NPS i ...
Hoag`s Object
... In the initial announcement of his discovery, Art Hoag proposed the hypothesis that the visible ring was a product of gravitational lensing. This idea was later discarded because the nucleus and the ring have the same redshift, and because more advanced telescopes revealed the knotty structure of th ...
... In the initial announcement of his discovery, Art Hoag proposed the hypothesis that the visible ring was a product of gravitational lensing. This idea was later discarded because the nucleus and the ring have the same redshift, and because more advanced telescopes revealed the knotty structure of th ...
Review Sheet and Study Hints - Tufts Institute of Cosmology
... Why do interacting/peculiar galaxies show such a wide spread of colors What are starburst galaxies Evolution and Formation Describe a theory about the formation of spirals. What evidence do we have for that? In what sense is the formation of ellipticals different from that of spirals? ...
... Why do interacting/peculiar galaxies show such a wide spread of colors What are starburst galaxies Evolution and Formation Describe a theory about the formation of spirals. What evidence do we have for that? In what sense is the formation of ellipticals different from that of spirals? ...
Test 1 - Brock physics
... 1. The mass of Star A is 5M , the mass of Star B is 4M , and the mass of Star C is 3M . The star with the longest lifetime on the main sequence is (a) Star A. (b) Star B. (c) Star C. (d) [There is not enough information.] 2. Very massive, hot stars are positioned in the ...
... 1. The mass of Star A is 5M , the mass of Star B is 4M , and the mass of Star C is 3M . The star with the longest lifetime on the main sequence is (a) Star A. (b) Star B. (c) Star C. (d) [There is not enough information.] 2. Very massive, hot stars are positioned in the ...
Chapter 19 Star Formation
... At stage 6, the core reaches 10 million K, and nuclear fusion begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. ...
... At stage 6, the core reaches 10 million K, and nuclear fusion begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. ...