Beyond the Solar System Homework for Geology 8
... 46. Although most dwarf stars are called white dwarfs, black dwarfs, or even brown dwarfs, these small stars can be additional colors as well, depending upon their surface temperatures. 47. Only the most massive stars evolve to become black dwarfs. 48. Hot stars evolve much more quickly than do cool ...
... 46. Although most dwarf stars are called white dwarfs, black dwarfs, or even brown dwarfs, these small stars can be additional colors as well, depending upon their surface temperatures. 47. Only the most massive stars evolve to become black dwarfs. 48. Hot stars evolve much more quickly than do cool ...
Mass Segregation in Globular Clusters
... One feature that characterizes such a cluster is that all its members should have approximately the same kinetic energy. For less massive stars, this means that on average, their velocities should be higher by a specific and measurable amount. ...
... One feature that characterizes such a cluster is that all its members should have approximately the same kinetic energy. For less massive stars, this means that on average, their velocities should be higher by a specific and measurable amount. ...
Astronomy (stars, galaxies and the Universe)
... Edwin Hubble discovered that almost all galaxies are moving away from us and from each other Hubble’s Law- the farther away a galaxy is, the faster it is moving away from us ...
... Edwin Hubble discovered that almost all galaxies are moving away from us and from each other Hubble’s Law- the farther away a galaxy is, the faster it is moving away from us ...
Exploration of the Milky Way and Nearby galaxies
... Higher resolution spectra with high S/N ratio needed for detailed chemical composition study to understand the origin and evolution is possible with TMT/HROS. An important source of observational constraints for studying s-process nucleosynthesis. ...
... Higher resolution spectra with high S/N ratio needed for detailed chemical composition study to understand the origin and evolution is possible with TMT/HROS. An important source of observational constraints for studying s-process nucleosynthesis. ...
Ch13_Lecture - Chemistry at Winthrop University
... groups according to their color (white, yellow, red, and deep red), which were subsequently subdivided into classes using the letters A through N ...
... groups according to their color (white, yellow, red, and deep red), which were subsequently subdivided into classes using the letters A through N ...
Astronomy (stars, galaxies and the Universe)
... gas revolving around a giant black hole in their centers ...
... gas revolving around a giant black hole in their centers ...
Beyond the Solar System Homework for Geology 8
... 46. Only the most massive stars evolve to become black holes. 47. Hot stars evolve much more rapidly than do cool stars. 48. Degenerate matter is highly condensed material, where even the electrons of atoms are pushed in, towards the center or nucleus of the atoms. 49. Pulsars are a type of neutron ...
... 46. Only the most massive stars evolve to become black holes. 47. Hot stars evolve much more rapidly than do cool stars. 48. Degenerate matter is highly condensed material, where even the electrons of atoms are pushed in, towards the center or nucleus of the atoms. 49. Pulsars are a type of neutron ...
Planetary Nebulae – White dwarfs
... Mostly made of Carbon and Oxygen No fusion to maintain heat and pressure to balance gravity pull ...
... Mostly made of Carbon and Oxygen No fusion to maintain heat and pressure to balance gravity pull ...
31Emission
... • Interstellar gas clouds can be heated by nearby stars, especially young hot ones • Atoms are excited by light from the stars and by collisions between atoms • When electrons fall down to lower energy levels, emission lines are produced ...
... • Interstellar gas clouds can be heated by nearby stars, especially young hot ones • Atoms are excited by light from the stars and by collisions between atoms • When electrons fall down to lower energy levels, emission lines are produced ...
University of Groningen Mass loss and rotational CO emission
... receivers are summarized in Table tab:efficiencies. Observations with the B3- and W-receivers were performed in double sideband (DSB) and dual polarization mode. The DSB mode was also used for the observations with the MPIfR/SRON E-band receiver. The bandwidth configuration of the receiver, and henc ...
... receivers are summarized in Table tab:efficiencies. Observations with the B3- and W-receivers were performed in double sideband (DSB) and dual polarization mode. The DSB mode was also used for the observations with the MPIfR/SRON E-band receiver. The bandwidth configuration of the receiver, and henc ...
Lecture6
... • Since all protostars of all mass range are born at roughly ~ 3000 K, with different luminosities, they all lie along the Hayashi Track on the HR Diagram. See Fig. II-56. (See class notes for the details.) • As the protostar keeps contracting and heats up, it moves on the H-R Diagram from the Haya ...
... • Since all protostars of all mass range are born at roughly ~ 3000 K, with different luminosities, they all lie along the Hayashi Track on the HR Diagram. See Fig. II-56. (See class notes for the details.) • As the protostar keeps contracting and heats up, it moves on the H-R Diagram from the Haya ...
Linking Asteroids and Meteorites through Reflectance
... • Because nuclear reactions have not yet begun in the protostar’s core, this luminosity is due entirely to the release of gravitational energy as the protostar continues to shrink and material from the surrounding fragment ...
... • Because nuclear reactions have not yet begun in the protostar’s core, this luminosity is due entirely to the release of gravitational energy as the protostar continues to shrink and material from the surrounding fragment ...
4. Massive Stars and HII Regions
... There are in principle two main ideas how very massive stars for: 1) like low mass stars via the collapse of a very massive dense cloud; this implies very high mass accretion rates; observationally one should be able to observe massive discs and outflows from those objects; 2) by coalescence of lowe ...
... There are in principle two main ideas how very massive stars for: 1) like low mass stars via the collapse of a very massive dense cloud; this implies very high mass accretion rates; observationally one should be able to observe massive discs and outflows from those objects; 2) by coalescence of lowe ...
Beyond the Solar System Homework for Geology 8
... stars can be additional colors as well, depending upon their surface temperatures. 46. Only the most massive stars evolve to become black dwarfs. 47. Hot stars evolve much more rapidly than do cool stars. 48. Degenerate matter is highly condensed material, where even the electrons of atoms are pushe ...
... stars can be additional colors as well, depending upon their surface temperatures. 46. Only the most massive stars evolve to become black dwarfs. 47. Hot stars evolve much more rapidly than do cool stars. 48. Degenerate matter is highly condensed material, where even the electrons of atoms are pushe ...
1/20/09 301 Physics Chapter 12 The Family of Stars Triangulation
... • Width of absorption line depends on density: wide for high density, narrow for low density ...
... • Width of absorption line depends on density: wide for high density, narrow for low density ...
Measuring Radii and Temperatures of Stars
... • To avoid uncertainties in Teff and BC • Determine PV as a function of B-V PV(B-V)=logTeff – 0.1BC PV ( B V ) a b( B V ) c( B V ) 2 d ( B V )3 ...
... • To avoid uncertainties in Teff and BC • Determine PV as a function of B-V PV(B-V)=logTeff – 0.1BC PV ( B V ) a b( B V ) c( B V ) 2 d ( B V )3 ...
Reach for the Stars B
... 7. Which DSO, a massive star-forming region, is depicted in Image [4]? 8. [T10] What is the common nickname of this DSO? 9. Which galaxy is this DSO located in? 10. Which DSO is the supermassive black hole at the center of the Milky Way? 11. How was it possible to determine the mass of this black ho ...
... 7. Which DSO, a massive star-forming region, is depicted in Image [4]? 8. [T10] What is the common nickname of this DSO? 9. Which galaxy is this DSO located in? 10. Which DSO is the supermassive black hole at the center of the Milky Way? 11. How was it possible to determine the mass of this black ho ...
Chapter 10: The Stars
... • Mystery Star A Star #3 and intensity graph B • Similarities in the number of spikes • Similar peak intensities (450 nm) • Mystery Star B Star #1/ graph C ...
... • Mystery Star A Star #3 and intensity graph B • Similarities in the number of spikes • Similar peak intensities (450 nm) • Mystery Star B Star #1/ graph C ...
Document
... • F Type: This type of star has a yellow-white color and surface temperatures between 6,000 K ﾑ 7,500 K. • G Type: These stars, with temperatures ranging between 5,000 K ﾑ 6,000 K, have spectra that betray the existence of ﾒmetalsﾓ or ﾒheavy elementsﾓ (any element heavier than Helium) and are yello ...
... • F Type: This type of star has a yellow-white color and surface temperatures between 6,000 K ﾑ 7,500 K. • G Type: These stars, with temperatures ranging between 5,000 K ﾑ 6,000 K, have spectra that betray the existence of ﾒmetalsﾓ or ﾒheavy elementsﾓ (any element heavier than Helium) and are yello ...
reach for the stars
... The mass of a star is inversely related to its expected lifespan. [The more massive the star is, the shorter its lifespan. The less massive the star is, the longer its lifespan.] 5. Why is this the case (referring to question #4)? (2 pts) Massive stars undergo more ...
... The mass of a star is inversely related to its expected lifespan. [The more massive the star is, the shorter its lifespan. The less massive the star is, the longer its lifespan.] 5. Why is this the case (referring to question #4)? (2 pts) Massive stars undergo more ...
Student Worksheet - Indiana University Astronomy
... young star cluster near its center. The dust lanes appear dark because they obscure visible light, and are thus seen in silhouette against the brighter, glowing, hydrogen gas. Surrounding the red nebula is a blue reflection nebula, especially bright at northern end. The reflection nebula glows by re ...
... young star cluster near its center. The dust lanes appear dark because they obscure visible light, and are thus seen in silhouette against the brighter, glowing, hydrogen gas. Surrounding the red nebula is a blue reflection nebula, especially bright at northern end. The reflection nebula glows by re ...
The Universe Section 1
... from the star’s center, and cooler gas sinks toward the center. – During radiation, atoms absorb energy and transfer it to other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
... from the star’s center, and cooler gas sinks toward the center. – During radiation, atoms absorb energy and transfer it to other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
HW11
... position that they do o the H-R diagram. For instance, red super giants have cool surface temperature. So they are on the right side of the diagram. But their luminosity is huge. This is because their radius is gigantic. 4) Understand spectral typing. Why the hydrogen lines become large as the surfa ...
... position that they do o the H-R diagram. For instance, red super giants have cool surface temperature. So they are on the right side of the diagram. But their luminosity is huge. This is because their radius is gigantic. 4) Understand spectral typing. Why the hydrogen lines become large as the surfa ...
Slide 1
... system. Both masses equal => center of mass is in the middle, rA = rB. The more unequal the masses are, the more it shifts toward the more massive star. ...
... system. Both masses equal => center of mass is in the middle, rA = rB. The more unequal the masses are, the more it shifts toward the more massive star. ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.