The star is born
... hydrogen gas and dust. The UV radiation from these O and B stars is ionizing the hydrogen atoms. The subsequent recombination of electrons and protons, with the electrons in excited states leads to the emission of visible light photons, mostly the red Balmer H-alpha transition. This is an example of ...
... hydrogen gas and dust. The UV radiation from these O and B stars is ionizing the hydrogen atoms. The subsequent recombination of electrons and protons, with the electrons in excited states leads to the emission of visible light photons, mostly the red Balmer H-alpha transition. This is an example of ...
Lesson Overviews and Content Standards
... This activity differs from the previous lessons in the set in that will not involve scale models. Rather, students will use a hands-on exercise in probability to learn about the relative number of main sequence stars of different classes (masses) that are born in a typical stellar nursery. An Intern ...
... This activity differs from the previous lessons in the set in that will not involve scale models. Rather, students will use a hands-on exercise in probability to learn about the relative number of main sequence stars of different classes (masses) that are born in a typical stellar nursery. An Intern ...
of the Sun
... • As the density was gradually reduced through expansion, matter began to form. • Both matter and anti-matter formed, but for some reason, there was a slight excess of matter. ...
... • As the density was gradually reduced through expansion, matter began to form. • Both matter and anti-matter formed, but for some reason, there was a slight excess of matter. ...
Time From the Perspective of a Particle Physicist
... If the temperature at the center becomes large enough (5 million degrees) then H to He fusion can occur: Star is born Many stars formed from same cloud ...
... If the temperature at the center becomes large enough (5 million degrees) then H to He fusion can occur: Star is born Many stars formed from same cloud ...
THE PHYSICAL CHARACTERIZATION OF THE STARS 1
... The stars are the basic pieces of the universe and the understanding of their properties, structure, formation and evolution is one of the most important branches of astrophysics. To characterize the stars allows to characterize the galaxies and from them the universe as a whole. As it is well known ...
... The stars are the basic pieces of the universe and the understanding of their properties, structure, formation and evolution is one of the most important branches of astrophysics. To characterize the stars allows to characterize the galaxies and from them the universe as a whole. As it is well known ...
Solar-like oscillations in intermediate red giants
... Helioseismology is currently the best method for verifying stellar evolution modelling theories and for understanding the structure and interior processes within the sun. It was able to rule out the possibility that the solar neutrino problem was due to incorrect models. ...
... Helioseismology is currently the best method for verifying stellar evolution modelling theories and for understanding the structure and interior processes within the sun. It was able to rule out the possibility that the solar neutrino problem was due to incorrect models. ...
Lec2015_22
... and cooling processes operative during collapse of gas cloud • A number of models have suggested that IMF would be skewed to much higher masses under such conditions – “Top heavy” • If low mass stars were formed, they should be detectable today • If only high-mass stars formed, then no Population II ...
... and cooling processes operative during collapse of gas cloud • A number of models have suggested that IMF would be skewed to much higher masses under such conditions – “Top heavy” • If low mass stars were formed, they should be detectable today • If only high-mass stars formed, then no Population II ...
I Cloudy with a Chance of Making a star is no easy thing
... one to 1,000 microns, or one millimeter. Matter with temperatures between three and 3,000 kelvins emits radiation that peaks in this band. Near-infrared radiation is the shortwavelength end of this range, roughly one to five microns. It is mostly starlight that has been modestly attenuated by dust. ...
... one to 1,000 microns, or one millimeter. Matter with temperatures between three and 3,000 kelvins emits radiation that peaks in this band. Near-infrared radiation is the shortwavelength end of this range, roughly one to five microns. It is mostly starlight that has been modestly attenuated by dust. ...
Lecture Eleven (Powerpoint format)
... Elliptical galaxies are distinguished by their Reddish light indicative of older stars Absence of current star formation Smooth centrally-condensed distribution of light, and absence of other ...
... Elliptical galaxies are distinguished by their Reddish light indicative of older stars Absence of current star formation Smooth centrally-condensed distribution of light, and absence of other ...
temperature - University of Texas Astronomy Home Page
... the stars are MOSTLY hydrogen (and helium) with trace levels of other elements. We only see those strong lines from the trace elements when there are variations in stellar temperature. ...
... the stars are MOSTLY hydrogen (and helium) with trace levels of other elements. We only see those strong lines from the trace elements when there are variations in stellar temperature. ...
What would the sky look like from the North Pole
... c) The image to the left shows a configuration in which the Sun is never to the zenith. Are there locations on Earth at which the Sun reaches the Zenith? If so, at what latitudes are they? At which time of the year do they reach the zenith? [hint: remember the tilt angle of the spin axis of the Eart ...
... c) The image to the left shows a configuration in which the Sun is never to the zenith. Are there locations on Earth at which the Sun reaches the Zenith? If so, at what latitudes are they? At which time of the year do they reach the zenith? [hint: remember the tilt angle of the spin axis of the Eart ...
– 1 – 1. Historical Notes for Ay 123 1.1.
... We now introduce the concept of proper motion, as stellar positions change through both parallax and proper motion, and astrometric programs seek to measure both of these.. Since stars move around with random motions within our Galaxy as well as rotate around its center, there are two components to ...
... We now introduce the concept of proper motion, as stellar positions change through both parallax and proper motion, and astrometric programs seek to measure both of these.. Since stars move around with random motions within our Galaxy as well as rotate around its center, there are two components to ...
Microlensing experiments Several experiments have searched for
... for microlensing events: • toward the Galactic Bulge (lenses are disk or bulge stars) • toward the Magellanic Clouds (lenses could be stars in the LMC / SMC, or halo objects) MACHO (Massive Compact Halo Object): • observed 11.9 million stars in the Large Magellanic Cloud for a total of 5.7 years. OG ...
... for microlensing events: • toward the Galactic Bulge (lenses are disk or bulge stars) • toward the Magellanic Clouds (lenses could be stars in the LMC / SMC, or halo objects) MACHO (Massive Compact Halo Object): • observed 11.9 million stars in the Large Magellanic Cloud for a total of 5.7 years. OG ...
Supernova - Mid-Pacific Institute
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
Star formation - Grosse Pointe Public School System
... Higher density regions of the ISM, often dark A giant molecular cloud: - 50 ly to 300 ly diameter - 100,000 to 10,000,000 solar masses - Higher Density than typical ISM - Temperature = 10 K to 30 K (cool enough for molecules to form) ...
... Higher density regions of the ISM, often dark A giant molecular cloud: - 50 ly to 300 ly diameter - 100,000 to 10,000,000 solar masses - Higher Density than typical ISM - Temperature = 10 K to 30 K (cool enough for molecules to form) ...
HR-diagram - Bakersfield College
... Magnitude is measured using (-) and (+) numbers the more (-) the number, the brighter the more (+), the dimmer the star ...
... Magnitude is measured using (-) and (+) numbers the more (-) the number, the brighter the more (+), the dimmer the star ...
Stellar Physics 1
... A. A hot dense gas produces a continuous spectrum with no spectral lines. B. A hot diffuse gas produces bright spectral lines – an emission spectrum. C. A cool dense gas produces a continuous spectrum with no spectral lines. y D. A cool diffuse gas in front of a source of continuous spectrum produce ...
... A. A hot dense gas produces a continuous spectrum with no spectral lines. B. A hot diffuse gas produces bright spectral lines – an emission spectrum. C. A cool dense gas produces a continuous spectrum with no spectral lines. y D. A cool diffuse gas in front of a source of continuous spectrum produce ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.