The dying sun/ creation of elements
... Supernova 1987A • Exploded in Large Magellanic Cloud • Small spiral galaxy that orbits our own Galaxy. ...
... Supernova 1987A • Exploded in Large Magellanic Cloud • Small spiral galaxy that orbits our own Galaxy. ...
Volume 2 (Issue 7), July 2013
... but some type of as yet unknown star-like objects. It also appeared that the radio emissions were coming from a pair of lobes surrounding these faint star-like objects. It was also discovered that these objects were located well outside our own galaxy. Quasars are very mysterious objects. Astronomer ...
... but some type of as yet unknown star-like objects. It also appeared that the radio emissions were coming from a pair of lobes surrounding these faint star-like objects. It was also discovered that these objects were located well outside our own galaxy. Quasars are very mysterious objects. Astronomer ...
Physics 1025: Lecture 17 Sun (cont.), Stellar Distances, Parallax
... the wavelength shift from the unshifted line λ. The star’s light will be blue-shifted if the star approaches earth. (Note in the case of an expanding nebula like the Crab Nebula, we assume it expands equally in all directions (i.e. spherically) and set VR= VT and can solve for the distance R to the ...
... the wavelength shift from the unshifted line λ. The star’s light will be blue-shifted if the star approaches earth. (Note in the case of an expanding nebula like the Crab Nebula, we assume it expands equally in all directions (i.e. spherically) and set VR= VT and can solve for the distance R to the ...
life
... •Visitors from outer space? •Fermi paradox – If they exist, why aren’t they here? •Travel to distant stars? •Search for signals from space? ...
... •Visitors from outer space? •Fermi paradox – If they exist, why aren’t they here? •Travel to distant stars? •Search for signals from space? ...
2 - Lnk2Lrn
... Stars Stars are formed by interstellar dust coming together through mutual gravitational attraction. The loss of potential energy is responsible for the initial high temperature necessary for fusion. The fusion process releases so much energy that the pressure created prevents the star from c ...
... Stars Stars are formed by interstellar dust coming together through mutual gravitational attraction. The loss of potential energy is responsible for the initial high temperature necessary for fusion. The fusion process releases so much energy that the pressure created prevents the star from c ...
High velocity clouds (v > 90 km/s), up to 108 M_sun in total Seen at
... High velocity clouds (v > 90 km/s), up to 108 M_sun in total! Seen at 21 cm, with high velocities up to 500 km/s. Mixed metallicity. ! Many partially ionized, and can contribute up to 1 M_sun/year (Lehner & Howk 2011)! ...
... High velocity clouds (v > 90 km/s), up to 108 M_sun in total! Seen at 21 cm, with high velocities up to 500 km/s. Mixed metallicity. ! Many partially ionized, and can contribute up to 1 M_sun/year (Lehner & Howk 2011)! ...
Part I Light, Telescopes, Atoms and Stars
... are missing) makes molecules – Within a single atom- the Coulomb force (positive charge attracts negative charge) holds the electrons to the atom = binding energy – The electrons ‘orbit’ at certain distances from the nucleus (a model!) – these orbitals have only certain ...
... are missing) makes molecules – Within a single atom- the Coulomb force (positive charge attracts negative charge) holds the electrons to the atom = binding energy – The electrons ‘orbit’ at certain distances from the nucleus (a model!) – these orbitals have only certain ...
Masses are much harder than distance, luminosity, or temperature
... • Range of different mass stars! ...
... • Range of different mass stars! ...
Evolution of a Star
... We have a theory of how stars evolve, what makes them different from one another and what happens when they die. Teachers - Stars begin as a large cloud of dust and gas called a nebula. The particles of dust and gas exert a gravitational force on each other causing the nebula to contract. As the par ...
... We have a theory of how stars evolve, what makes them different from one another and what happens when they die. Teachers - Stars begin as a large cloud of dust and gas called a nebula. The particles of dust and gas exert a gravitational force on each other causing the nebula to contract. As the par ...
The physics of high-mass star formation
... IMF high-mass stars are rare: N(1 MO) = 100 N(10 MO) large distance: >400 pc, typically a few kpc formation in clusters confusion ...
... IMF high-mass stars are rare: N(1 MO) = 100 N(10 MO) large distance: >400 pc, typically a few kpc formation in clusters confusion ...
Supernova - Mid-Pacific Institute
... collapse and in so doing will release a huge amount of energy. This will cause a blast wave that ejects the star's envelope into interstellar space. ...
... collapse and in so doing will release a huge amount of energy. This will cause a blast wave that ejects the star's envelope into interstellar space. ...
seven winter constellations
... Orion (uh-rye-un) was a famous hunter who bragged that he could kill all of the animals in the world. The gods decided to teach the hunter a lesson by sending the giant scorpion, Scorpius, to sting Orion while he was hunting a hare. Then, as an example to all mortals, the gods placed Orion, Lepus (t ...
... Orion (uh-rye-un) was a famous hunter who bragged that he could kill all of the animals in the world. The gods decided to teach the hunter a lesson by sending the giant scorpion, Scorpius, to sting Orion while he was hunting a hare. Then, as an example to all mortals, the gods placed Orion, Lepus (t ...
Basic Properties of Stars
... Hertzsprung-Russell Diagram Beware of the selection effects in the HR Diagram HR diagram of the brightest stars in the night sky. HR diagram of the stars nearest to the Sun. ...
... Hertzsprung-Russell Diagram Beware of the selection effects in the HR Diagram HR diagram of the brightest stars in the night sky. HR diagram of the stars nearest to the Sun. ...
The Reflector: January 2010 - Peterborough Astronomical Association
... star birthing area in Sagittarius to two double stars in Cygnus, a million stars in a ball in Hercules, and finally to the final stages of star life in M57 and M27, all in one night. It’s quite a story and you’ll meet a red giant star—Antares—along the way. Planet buffs will also be able to take in ...
... star birthing area in Sagittarius to two double stars in Cygnus, a million stars in a ball in Hercules, and finally to the final stages of star life in M57 and M27, all in one night. It’s quite a story and you’ll meet a red giant star—Antares—along the way. Planet buffs will also be able to take in ...
1:45 PM TuTh This is a one-quarter course on
... STARS AND STELLAR EVOLUTION, WINTER, 2014 Physical Sciences 130; 12 - 1:45 PM TuTh This is a one-quarter course on stars, stellar evolution, and topics known collectively as ``high energy astrophysics'' as it applies to stellar phenomena. Thus the subject matter includes, in addition to the study of ...
... STARS AND STELLAR EVOLUTION, WINTER, 2014 Physical Sciences 130; 12 - 1:45 PM TuTh This is a one-quarter course on stars, stellar evolution, and topics known collectively as ``high energy astrophysics'' as it applies to stellar phenomena. Thus the subject matter includes, in addition to the study of ...
Young Stellar Objects in the Orion B Cloud
... interesting is the frequency mass distribution of the YSOs, i.e., the shape of the mass function, and, related to this, the number of substellar sources. Even though a number of surveys of different star formation regions have been carried out over the last decade, there is still an ongoing debate o ...
... interesting is the frequency mass distribution of the YSOs, i.e., the shape of the mass function, and, related to this, the number of substellar sources. Even though a number of surveys of different star formation regions have been carried out over the last decade, there is still an ongoing debate o ...
Solutions
... will be the brightest ones. All the stars in a globular cluster are very close to being at the same distance from us, so the most luminous ones are the ones that will appear brightest. Note: A number of you said that red giants were the brighest because they are very massive and very luminous. They ...
... will be the brightest ones. All the stars in a globular cluster are very close to being at the same distance from us, so the most luminous ones are the ones that will appear brightest. Note: A number of you said that red giants were the brighest because they are very massive and very luminous. They ...
Reach for the Stars B
... 20. Which portion of the EM spectrum was this image taken in? 21. Which DSO is depicted in Image [7]? 22. What is special about the stars forming here? 23. Which DSO is depicted in Image [8]? 24. Stars like this DSO can undergo sudden outbursts where their brightness varies wildly. What are they cal ...
... 20. Which portion of the EM spectrum was this image taken in? 21. Which DSO is depicted in Image [7]? 22. What is special about the stars forming here? 23. Which DSO is depicted in Image [8]? 24. Stars like this DSO can undergo sudden outbursts where their brightness varies wildly. What are they cal ...
xam2ans
... (c) Consider this weak reaction: p+ + e → n + e . Why does it almost never occur in the core of a main sequence star like the Sun? Answer: The rest mass energy of a neutron is larger than a proton plus electron. Consequently this reaction is endothermic, which means energetically unfavorable. (d) ...
... (c) Consider this weak reaction: p+ + e → n + e . Why does it almost never occur in the core of a main sequence star like the Sun? Answer: The rest mass energy of a neutron is larger than a proton plus electron. Consequently this reaction is endothermic, which means energetically unfavorable. (d) ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... Windows PCs. Link from module page on QOL. Animates the evolution of stars (0.8 to 25 solar masses, solar metallicity) in the Hertzsprung-Russell (H-R) diagram, more exactly in the log(L/L) vs. log(Teff/K) plane. The evolution is followed from the initial main sequence (also called zero age main se ...
... Windows PCs. Link from module page on QOL. Animates the evolution of stars (0.8 to 25 solar masses, solar metallicity) in the Hertzsprung-Russell (H-R) diagram, more exactly in the log(L/L) vs. log(Teff/K) plane. The evolution is followed from the initial main sequence (also called zero age main se ...
How big are stars? How do we know?
... Most of the brightest stars in the sky are a) relatively hot main-sequence stars that are relatively close to the Sun. b) relatively cool giant stars that are relatively close to the Sun. c) relatively cool main-sequence stars that are relatively far from the Sun. d) relatively cool main-sequence s ...
... Most of the brightest stars in the sky are a) relatively hot main-sequence stars that are relatively close to the Sun. b) relatively cool giant stars that are relatively close to the Sun. c) relatively cool main-sequence stars that are relatively far from the Sun. d) relatively cool main-sequence s ...
mslien~1
... Out of deep images & with the detection 20 of stars on 5 level Succeeded to detected very faint (low mass) stars ...
... Out of deep images & with the detection 20 of stars on 5 level Succeeded to detected very faint (low mass) stars ...
Staring Back to Cosmic Dawn - UC-HiPACC
... The Case of the Chaotic Blue Galaxies Ever since Hubble’s first spectacular images of distant galaxies, an enduring puzzle has been why early starforming galaxies look much more irregular and jumbled than nearby blue galaxies. Nearby blue galaxies are relatively smooth. The most beautiful ones are e ...
... The Case of the Chaotic Blue Galaxies Ever since Hubble’s first spectacular images of distant galaxies, an enduring puzzle has been why early starforming galaxies look much more irregular and jumbled than nearby blue galaxies. Nearby blue galaxies are relatively smooth. The most beautiful ones are e ...
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.