Student Exploration Sheet: Growing Plants
... A nebula is an enormous cloud of gas and dust in which stars are born. Most nebulae produce an emission spectrum, which is characterized by bright lines of color against a dark background. The bright lines in an emission spectrum correspond to the dark lines in an absorption spectrum. ...
... A nebula is an enormous cloud of gas and dust in which stars are born. Most nebulae produce an emission spectrum, which is characterized by bright lines of color against a dark background. The bright lines in an emission spectrum correspond to the dark lines in an absorption spectrum. ...
DTU 8e Chap 11 Characterizing Stars
... These diagrams show the relationship between the color of a star and its surface temperature. The intensity of light emitted by three stars is plotted against wavelength. The range of visible wavelengths is indicated. The location of the peak of each star’s intensity curve, relative to the visible-l ...
... These diagrams show the relationship between the color of a star and its surface temperature. The intensity of light emitted by three stars is plotted against wavelength. The range of visible wavelengths is indicated. The location of the peak of each star’s intensity curve, relative to the visible-l ...
Properties of Stars - Montana State University Extended University
... The strength and pattern of the absorption lines does vary among the stars. Some stars have strong (dark) hydrogen lines, other stars have no hydrogen lines but strong calcium and sodium lines. Are their abundances different? No. When scientists learned more about the physics of the atom, they disco ...
... The strength and pattern of the absorption lines does vary among the stars. Some stars have strong (dark) hydrogen lines, other stars have no hydrogen lines but strong calcium and sodium lines. Are their abundances different? No. When scientists learned more about the physics of the atom, they disco ...
doc - Jnoodle
... In the center we have the sun, our closest star. There are so far 9 known planets, of which the 5 inner have been known since ancient times, Uranus was discovered in the 18th and Neptune in the 19th century, Pluto as late as 1930. The gravitational disturbances on the orbits of thus far known planet ...
... In the center we have the sun, our closest star. There are so far 9 known planets, of which the 5 inner have been known since ancient times, Uranus was discovered in the 18th and Neptune in the 19th century, Pluto as late as 1930. The gravitational disturbances on the orbits of thus far known planet ...
The Fundamental Plane, Stellar Popula6ons
... What is origin of the ‘Blt’ of the FP and its variaBon with λ? How much is due to stellar populaBon variaBons and how much is due to structural non‐homology or variaBons in Mstar/Mdark? What is the origin of the sca7er about the FP? Are there extra (hidden) parameters or is it due to the ...
... What is origin of the ‘Blt’ of the FP and its variaBon with λ? How much is due to stellar populaBon variaBons and how much is due to structural non‐homology or variaBons in Mstar/Mdark? What is the origin of the sca7er about the FP? Are there extra (hidden) parameters or is it due to the ...
Hall Scorpius constellation (11) Jacob Hall Physics 1040, sec 002
... and at an estimated distance of 32,600 light-years, M80's spatial diameter is about 95 light-years. It contains several hundred thousand stars, and is among the more densely populated globular clusters in the Milky Way Galaxy. M80 contains a relatively large number of blue stragglers, stars that app ...
... and at an estimated distance of 32,600 light-years, M80's spatial diameter is about 95 light-years. It contains several hundred thousand stars, and is among the more densely populated globular clusters in the Milky Way Galaxy. M80 contains a relatively large number of blue stragglers, stars that app ...
Origin of the Elements
... silicon (Si) are formed in the outer layers. The heavier elements are formed closer to the core and eventually fuse in the core of the star to form iron (Fe), the most massive element found in stars. ...
... silicon (Si) are formed in the outer layers. The heavier elements are formed closer to the core and eventually fuse in the core of the star to form iron (Fe), the most massive element found in stars. ...
The Physics of Massive Star Formation
... with vir ≈ 1, flat bottom ( const in center) Result: most mass goes into a single object ...
... with vir ≈ 1, flat bottom ( const in center) Result: most mass goes into a single object ...
Chapter 12
... ionized state • A stars have just the right temperature to put electrons into hydrogen’s 2nd energy level, which results in strong absorption lines in the visible • F, G, and K stars are of a low enough temperature to show absorption lines of metals such as calcium and iron, elements that are typica ...
... ionized state • A stars have just the right temperature to put electrons into hydrogen’s 2nd energy level, which results in strong absorption lines in the visible • F, G, and K stars are of a low enough temperature to show absorption lines of metals such as calcium and iron, elements that are typica ...
THE STARS G. Iafrate(a), M. Ramella(a) and V. Bologna(b) (a) INAF
... luminosity but low temperature. The white dwarfs, that are very hot but small, lie in the lower left corner of the diagram. Stellar evolution Stars are big spheres of gas (if the planet Earth is a grain of sand, a medium size star is a ball of 1 meter diameter). Stars produce energy by nuclear fusio ...
... luminosity but low temperature. The white dwarfs, that are very hot but small, lie in the lower left corner of the diagram. Stellar evolution Stars are big spheres of gas (if the planet Earth is a grain of sand, a medium size star is a ball of 1 meter diameter). Stars produce energy by nuclear fusio ...
the stars - Uni Heidelberg
... parameters temperature and luminosity. By selecting stars on the sky you build the Herzsprung-Russell diagram that shows the relation between color and magnitude, a milestone in the history of our understanding of how stars work and evolve. If used in the classroom, the meaning of temperature, color ...
... parameters temperature and luminosity. By selecting stars on the sky you build the Herzsprung-Russell diagram that shows the relation between color and magnitude, a milestone in the history of our understanding of how stars work and evolve. If used in the classroom, the meaning of temperature, color ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... Through Spitzer and XMM-Newton we identify ∼ 702 PMS stars that emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean ...
... Through Spitzer and XMM-Newton we identify ∼ 702 PMS stars that emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean ...
CONSTELLATION CASSIOPEIA named after the
... NGC 457 is looser and NGC 457 is arrayed in chains, approximately 10,000 light-years from Earth. IC 289 is a Planetary nebula cloud of ionised gas being pushed out into space by the remnants of the star’s core. There are two supernova remnants in Cassiopeia. The first is the aftermath of the supern ...
... NGC 457 is looser and NGC 457 is arrayed in chains, approximately 10,000 light-years from Earth. IC 289 is a Planetary nebula cloud of ionised gas being pushed out into space by the remnants of the star’s core. There are two supernova remnants in Cassiopeia. The first is the aftermath of the supern ...
DTU 8e Chap 17 Quasars and Other Active Galaxies
... An active galaxy is an extremely luminous galaxy that has one or more unusual features: an unusually bright, starlike nucleus; strong emission lines in its spectrum; rapid variations in luminosity; and jets or beams of radiation that emanate from its core. Active galaxies include quasars, Seyfert ga ...
... An active galaxy is an extremely luminous galaxy that has one or more unusual features: an unusually bright, starlike nucleus; strong emission lines in its spectrum; rapid variations in luminosity; and jets or beams of radiation that emanate from its core. Active galaxies include quasars, Seyfert ga ...
Activity in other Stars I
... Spicules are formed by sound waves, which have a period of about 5minutes. Although the sound waves usually are damped, under certain conditions, they leak into the low atmosphere, or Chromosphere, spawning shock waves. ...
... Spicules are formed by sound waves, which have a period of about 5minutes. Although the sound waves usually are damped, under certain conditions, they leak into the low atmosphere, or Chromosphere, spawning shock waves. ...
PRESENT-DAY CLUSTER FORMATION
... full content and extent of the Trapezium cluster have become apparent only with the advent of infrared array photographs, which have shown that it contains more than 500 stars in a highly centrally concentrated and approximately symmetrical distribution centered on the Trapezium (McCaughrean 1989; M ...
... full content and extent of the Trapezium cluster have become apparent only with the advent of infrared array photographs, which have shown that it contains more than 500 stars in a highly centrally concentrated and approximately symmetrical distribution centered on the Trapezium (McCaughrean 1989; M ...
Syllabus - University of Texas Rio Grande Valley
... State the three main types of galaxies. State the two main components of spiral galaxies (disk, spheroidal). State the two main parts of the spheroidal component of spiral galaxies (bulge, halo). State which type(s) of galaxies present a spheroidal component. State the different methods used to dete ...
... State the three main types of galaxies. State the two main components of spiral galaxies (disk, spheroidal). State the two main parts of the spheroidal component of spiral galaxies (bulge, halo). State which type(s) of galaxies present a spheroidal component. State the different methods used to dete ...
SMMP_BISANA - Infinity and Beyond
... Young stars emit jets of intense radiation that heat the surrounding matter to the point at which it glows brightly. These narrowly-focused jets can be trillions of miles long and can travel at 500,000 miles per hour. These jets may be focused by the star's magnetic field. The protostar is now a st ...
... Young stars emit jets of intense radiation that heat the surrounding matter to the point at which it glows brightly. These narrowly-focused jets can be trillions of miles long and can travel at 500,000 miles per hour. These jets may be focused by the star's magnetic field. The protostar is now a st ...
Power Point Presentation
... Universe has collapsed due to a slightly higher density of dark matter. It forms a 100 million solar mass protogalaxy, and at the center of this protogalaxy, a star is born! Density movie ...
... Universe has collapsed due to a slightly higher density of dark matter. It forms a 100 million solar mass protogalaxy, and at the center of this protogalaxy, a star is born! Density movie ...
Document
... • Interstellar gas clouds emit intense microwaves at specific frequencies. • Doppler shift gives speed • True speed plus proper motion gives distance • Maybe 10s of Mpc but new technique ...
... • Interstellar gas clouds emit intense microwaves at specific frequencies. • Doppler shift gives speed • True speed plus proper motion gives distance • Maybe 10s of Mpc but new technique ...
The colours of the Universe, the amateur astronomical spectroscopy.
... bright giants. On the graph of this there star are presented some absorption lines of chemical elements such as: Balmer's hydrogen spectral series, helium, nitrogen and carbon, which prove their presence in the Mintaka's chromospheres. In the stars of high temperature, spectral type O, there are ion ...
... bright giants. On the graph of this there star are presented some absorption lines of chemical elements such as: Balmer's hydrogen spectral series, helium, nitrogen and carbon, which prove their presence in the Mintaka's chromospheres. In the stars of high temperature, spectral type O, there are ion ...
society journal - Auckland Astronomical Society
... delays mean a change of target. This meant putting the probe into hibernation for several years and then bring all the equipment back to life. Gravity of just 1000 of Earths required making a lander that could be anchored on to the surface of the comet. The second film, which was a sky at night spec ...
... delays mean a change of target. This meant putting the probe into hibernation for several years and then bring all the equipment back to life. Gravity of just 1000 of Earths required making a lander that could be anchored on to the surface of the comet. The second film, which was a sky at night spec ...
observation reports
... selection of open clusters, and ending with the glorious M11 in Scutum, which revealed about 80-100 stars in the field at high power. 23:05 (00:05) Time to take a break from the ETX, for a naked-eye look at the sky. The Milky Way was visible all the way from Perseus to Scutum, and very clear in Cygn ...
... selection of open clusters, and ending with the glorious M11 in Scutum, which revealed about 80-100 stars in the field at high power. 23:05 (00:05) Time to take a break from the ETX, for a naked-eye look at the sky. The Milky Way was visible all the way from Perseus to Scutum, and very clear in Cygn ...
Spatial distribution of stars in the Milky Way
... Item 4) is a lower limit, since objects such as white dwarfs, neutron stars, etc, do contribute to the total mass budget, but virtually no light. ...
... Item 4) is a lower limit, since objects such as white dwarfs, neutron stars, etc, do contribute to the total mass budget, but virtually no light. ...
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.