Stars I - Astronomy Centre
... in the Sun, yet Jupiter, with 1/1000 of Sun’s mass, possesses more angular momentum than any other body including the Sun. Why? ...
... in the Sun, yet Jupiter, with 1/1000 of Sun’s mass, possesses more angular momentum than any other body including the Sun. Why? ...
New light on our Sun`s fate - Space Telescope Science Institute
... “catch me if you can” game with our star. As the Sun loses mass, and hence gravitational influence, Earth’s orbit will expand to some 50 percent farther out than it currently is. Unfortunately for our planet, the Sun will lose mass rapidly as a red giant, and its outer layers will overtake Earth’s m ...
... “catch me if you can” game with our star. As the Sun loses mass, and hence gravitational influence, Earth’s orbit will expand to some 50 percent farther out than it currently is. Unfortunately for our planet, the Sun will lose mass rapidly as a red giant, and its outer layers will overtake Earth’s m ...
Stars, Galaxies, and the Universe Section 1 Section 1
... • Most stars have several types of actual motion. • Stars move across the sky (seen only for close stars). • Some stars may revolve around another star. • Stars either move away from or toward our solar system. ...
... • Most stars have several types of actual motion. • Stars move across the sky (seen only for close stars). • Some stars may revolve around another star. • Stars either move away from or toward our solar system. ...
D2 Stellar characteristics and stellar evolution
... ▪ fusing hydrogen into helium, the difference between them is in mass ▪ during the lifetime of a star its position will move on the diagram as its temperature and luminosity changes ▪ left upper corner more massive than right lower corner ▪ cooler red stars relatively low luminosity; ▪ hotter blue s ...
... ▪ fusing hydrogen into helium, the difference between them is in mass ▪ during the lifetime of a star its position will move on the diagram as its temperature and luminosity changes ▪ left upper corner more massive than right lower corner ▪ cooler red stars relatively low luminosity; ▪ hotter blue s ...
File - YEAR 11 EBSS PHYSICS DETAILED STUDIES
... Stars come in many colours… By looking at the apparent brightness of three different spectra, Ultraviolet (U), Violet-Blue (B) and Visible (V) we can determine the surface temperature of a star. This can be done by taking a ratio of the brightness in V (bV) to the brightness in B (bB). A hot star ...
... Stars come in many colours… By looking at the apparent brightness of three different spectra, Ultraviolet (U), Violet-Blue (B) and Visible (V) we can determine the surface temperature of a star. This can be done by taking a ratio of the brightness in V (bV) to the brightness in B (bB). A hot star ...
1 Introduction - High Point University
... That was not the case however, for the Hertzsprung-Russell diagram. A significant tool to aid in the understanding of stellar evolution, the H-R diagram was discovered independently by two astronomers in 1912 using observational comparisons. They found that when stars are plotted using the propertie ...
... That was not the case however, for the Hertzsprung-Russell diagram. A significant tool to aid in the understanding of stellar evolution, the H-R diagram was discovered independently by two astronomers in 1912 using observational comparisons. They found that when stars are plotted using the propertie ...
Stellar Evolution Chapter 12
... b. Objects below this mass can only form in HI clouds. c. Objects below this mass are not hot enough to fuse normal hydrogen. d. They form too slowly and hot stars nearby clear the gas and dust quickly. e. Our telescopes do not have enough light gathering power to detect dim objects. ...
... b. Objects below this mass can only form in HI clouds. c. Objects below this mass are not hot enough to fuse normal hydrogen. d. They form too slowly and hot stars nearby clear the gas and dust quickly. e. Our telescopes do not have enough light gathering power to detect dim objects. ...
Life cycle of low mass stars
... weigh 100 million tons High temperature but not very bright. Gravity > internal pressure Option 2: 6b. Black hole Black hole = objects smaller and more dense than Neutron stars. Created by massive Red Supergiants. Pull of gravity is so great that not even light can escape. Gravity >internal pressure ...
... weigh 100 million tons High temperature but not very bright. Gravity > internal pressure Option 2: 6b. Black hole Black hole = objects smaller and more dense than Neutron stars. Created by massive Red Supergiants. Pull of gravity is so great that not even light can escape. Gravity >internal pressure ...
Amanda Boyle Starstuff
... Stars come into existence when they begin to fuel their existence with fusion. The biggest and most luminous stars are born first, and there are only a few of these O and B Stars. As you go down the line, more and more of each kind exist with the most common being M. Our Sun is a G. Not as in a gan ...
... Stars come into existence when they begin to fuel their existence with fusion. The biggest and most luminous stars are born first, and there are only a few of these O and B Stars. As you go down the line, more and more of each kind exist with the most common being M. Our Sun is a G. Not as in a gan ...
b. false - UW Canvas
... good representation of how stars “work,” we would conclude that a. the hotter the star is, the more luminous it is, and the brighter the colors will be overall. b. the cooler the star, the less luminous it is; the brighter part of the spectrum will be toward longer wavelengths. c. the luminosity of ...
... good representation of how stars “work,” we would conclude that a. the hotter the star is, the more luminous it is, and the brighter the colors will be overall. b. the cooler the star, the less luminous it is; the brighter part of the spectrum will be toward longer wavelengths. c. the luminosity of ...
Starspots (AIP – Klaus G
... Magnetic fields likely play an important role in almost any astrophysical target, from the early Universe to the Sun, Earth, and its environment. While numerical 3-D MHD simulations became more and more sophisticated in the previous years, magnetic-field observations are still extremely rare (except ...
... Magnetic fields likely play an important role in almost any astrophysical target, from the early Universe to the Sun, Earth, and its environment. While numerical 3-D MHD simulations became more and more sophisticated in the previous years, magnetic-field observations are still extremely rare (except ...
“Crossroads of Astronomy.” Talk about Five Remarkable
... Classified 5,000 stars per month between 1911 and 1915. She would examine the photographic plate and call out a letter for each spectrum to an assistant. Annie achieved a rate of more than 3 stars a minute. Annie used Williamina Fleming’s system, rearranged it, and introduced decimal subdivisions. T ...
... Classified 5,000 stars per month between 1911 and 1915. She would examine the photographic plate and call out a letter for each spectrum to an assistant. Annie achieved a rate of more than 3 stars a minute. Annie used Williamina Fleming’s system, rearranged it, and introduced decimal subdivisions. T ...
answers2006_07_BC
... Type Ia supernovae all have very similar brightness, and are bright enough to be seen out to large redshifts, so can be used to check how the expansion of the universe changes with time. ...
... Type Ia supernovae all have very similar brightness, and are bright enough to be seen out to large redshifts, so can be used to check how the expansion of the universe changes with time. ...
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 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 ...
Deep Space (PDF: 224k)
... Stars with initial masses between eight and 50 times that of the Sun do not evolve to the Wolf-Rayet stage; they never completely lose the hydrogen in their outer layers. Such stars also become blue and red supergiants. As they build up an iron core, they too explode as supernovae. The remaining cor ...
... Stars with initial masses between eight and 50 times that of the Sun do not evolve to the Wolf-Rayet stage; they never completely lose the hydrogen in their outer layers. Such stars also become blue and red supergiants. As they build up an iron core, they too explode as supernovae. The remaining cor ...
DO NOW - PBworks
... The student is expected to explore how different wavelengths of the electromagnetic spectrum such as light and radio waves are used to gain information about distances and properties of components in the universe. ...
... The student is expected to explore how different wavelengths of the electromagnetic spectrum such as light and radio waves are used to gain information about distances and properties of components in the universe. ...
What we can measure
... measuring how much red versus how much blue there is in the spectra of the star. Thus we refer to the cooler stars as “red” stars and the hotter stars as “blue” stars. But we have developed a letter scale for this as well: From hotter to cooler we have: O B A F G K M (O stars are the hottest and blu ...
... measuring how much red versus how much blue there is in the spectra of the star. Thus we refer to the cooler stars as “red” stars and the hotter stars as “blue” stars. But we have developed a letter scale for this as well: From hotter to cooler we have: O B A F G K M (O stars are the hottest and blu ...
30.2 PowerPoint Stellar Evolution
... the core of the star The energy from fusion balances the force of gravity and makes it a very stable stage ...
... the core of the star The energy from fusion balances the force of gravity and makes it a very stable stage ...
about Stars
... of B-V color, and are found on the left side of the diagram. Cooler stars are brighter in yellow light than in blue light, have larger values of B-V color, and are found on the right side of the diagram. ...
... of B-V color, and are found on the left side of the diagram. Cooler stars are brighter in yellow light than in blue light, have larger values of B-V color, and are found on the right side of the diagram. ...
N5128PNSydney
... 0.1-10Gyr depending on initial mass, following the red-giant branch (RGB) and asymptotic giant branch (AGB) to the white dwarf cooling track Length of PN phase ~104 yr (depending on core mass) Emission from the expanding shell ionized by the hot (50-150,000 K) central star Ionization level falls wit ...
... 0.1-10Gyr depending on initial mass, following the red-giant branch (RGB) and asymptotic giant branch (AGB) to the white dwarf cooling track Length of PN phase ~104 yr (depending on core mass) Emission from the expanding shell ionized by the hot (50-150,000 K) central star Ionization level falls wit ...
Distance, Size, and Temperature of a Star
... after billions and maybe even trillions of years, it will stop glowing and at that point, it will be what we call a black dwarf star. There are still no black dwarf stars in the Universe. Blue Giant Stars: Because blue stars are large, and compact, they burn their fuel quickly, which gives them a v ...
... after billions and maybe even trillions of years, it will stop glowing and at that point, it will be what we call a black dwarf star. There are still no black dwarf stars in the Universe. Blue Giant Stars: Because blue stars are large, and compact, they burn their fuel quickly, which gives them a v ...
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.