Star Formation
... core temperature rises above 107 K. • Thermal pressure cannot stop contraction because the star is constantly losing thermal energy from its surface through radiation • Is there another form of pressure that can stop contraction? ...
... core temperature rises above 107 K. • Thermal pressure cannot stop contraction because the star is constantly losing thermal energy from its surface through radiation • Is there another form of pressure that can stop contraction? ...
G-stars - Gemini Astronomie
... dust, mostly from the death of older stars. Due to the force of its own gravity, the cloud begins to collapse inward when the temperature of the cloud has cooled down to about 10 K! Then every atom and every bit of dust is pulled to the center to build a protostar. The atoms speed up by increasing g ...
... dust, mostly from the death of older stars. Due to the force of its own gravity, the cloud begins to collapse inward when the temperature of the cloud has cooled down to about 10 K! Then every atom and every bit of dust is pulled to the center to build a protostar. The atoms speed up by increasing g ...
Chapter 9 “The Family of Stars “
... Mars' orbit is larger than Earth's, and stars would show a larger parallax when observed from Mars as compared to Earth. We would be able to determine the distance to nearby stars more accurately and determine the distance to stars that are currently too far to be measured using parallax from Earth. ...
... Mars' orbit is larger than Earth's, and stars would show a larger parallax when observed from Mars as compared to Earth. We would be able to determine the distance to nearby stars more accurately and determine the distance to stars that are currently too far to be measured using parallax from Earth. ...
ASTR3007/4007/6007, Class 1: Observing the Stars 23 February
... massive, while M stars are the least massive. O stars are also the largest. The Sun is a G star. In modern times observations have gotten better, and we can now see objects too dim and cool to be stars. These are called brown dwarfs, and two new spectral types have been added to cover them. These ar ...
... massive, while M stars are the least massive. O stars are also the largest. The Sun is a G star. In modern times observations have gotten better, and we can now see objects too dim and cool to be stars. These are called brown dwarfs, and two new spectral types have been added to cover them. These ar ...
Name:
... 9. Where in the H-R diagram would you find the sun the same size and color as our sun? (Click here and there around the diagram until the two stars in the upper left box are the same in terms of color and size.) upper left ...
... 9. Where in the H-R diagram would you find the sun the same size and color as our sun? (Click here and there around the diagram until the two stars in the upper left box are the same in terms of color and size.) upper left ...
Star Basics
... the hydrogen lines are weak. Both HeI and HeII (singly ionized helium) are seen in the higher temperature examples. The radiation from O5 stars is so intense that it can ionize hydrogen over a volume of space 1000 light years across. One example is the luminous H II region surrounding star cluster M ...
... the hydrogen lines are weak. Both HeI and HeII (singly ionized helium) are seen in the higher temperature examples. The radiation from O5 stars is so intense that it can ionize hydrogen over a volume of space 1000 light years across. One example is the luminous H II region surrounding star cluster M ...
test - Scioly.org
... dwarf-type star, cooler than the Sun, while the other is a white dwarf, the stms are so close that they complete their orbital revolution in slightly over 6 1/2 hours and have a light curve illustrated in figure #2 D) SN 2Ollfe A) HM Cancri E) NGC 1846 B) SS Cvpi ...
... dwarf-type star, cooler than the Sun, while the other is a white dwarf, the stms are so close that they complete their orbital revolution in slightly over 6 1/2 hours and have a light curve illustrated in figure #2 D) SN 2Ollfe A) HM Cancri E) NGC 1846 B) SS Cvpi ...
PHYSICS 1500 - ASTRONOMY TOTAL: 100 marks Section A Please
... (a) These are clearly the most common type of planet. (b) Smaller, rocky planets always lie closer to the star but are undetectable. (c) Few planetary systems have giant planets more than 1 AU from the star. (d) Detection of less massive planets is currently very difficult. (e) Detection of planets ...
... (a) These are clearly the most common type of planet. (b) Smaller, rocky planets always lie closer to the star but are undetectable. (c) Few planetary systems have giant planets more than 1 AU from the star. (d) Detection of less massive planets is currently very difficult. (e) Detection of planets ...
4P38.pdf
... studies of K and M main-sequence stars have revealed that they have very strong coronal/chromospheric XUV emission fluxes compared to solar-type with similar rotation periods or ages. This enhanced XUV radiation environment is expected to play a major role in the development of the atmospheres and u ...
... studies of K and M main-sequence stars have revealed that they have very strong coronal/chromospheric XUV emission fluxes compared to solar-type with similar rotation periods or ages. This enhanced XUV radiation environment is expected to play a major role in the development of the atmospheres and u ...
8.1 Stars
... attraction of a nearby star or the shockwave from an exploding star. The area with the largest mass starts to pull more mass in. The matter pulled in has excess energy which causes the central ball of material to begin to spin. Extremely high pressures build up inside the ball, which in turn cause ...
... attraction of a nearby star or the shockwave from an exploding star. The area with the largest mass starts to pull more mass in. The matter pulled in has excess energy which causes the central ball of material to begin to spin. Extremely high pressures build up inside the ball, which in turn cause ...
elementary measuring stars
... H-R Diagram. The figure used by Ejnar Hertzsprung and Henry Norris Russell to demonstrate how luminosity relates to temperature in stars. Stefan-Boltzmann Law. The relation describing how a star’s luminosity depends on its surface area and temperature. Dwarf. The term used to describe stars populati ...
... H-R Diagram. The figure used by Ejnar Hertzsprung and Henry Norris Russell to demonstrate how luminosity relates to temperature in stars. Stefan-Boltzmann Law. The relation describing how a star’s luminosity depends on its surface area and temperature. Dwarf. The term used to describe stars populati ...
The Stars: Distance, Luminosity, Size
... The more massive a Main Sequence star is, the hotter (bluer), and more luminous. The Main Sequence is a mass sequence! ...
... The more massive a Main Sequence star is, the hotter (bluer), and more luminous. The Main Sequence is a mass sequence! ...
Week 11 Concept Summary
... (c) Halo: The halo contains only older stars, almost all inside the globular clusters also found there. There is no gas and dust, and what stars are there have very low concentrations of heavy elements. They also orbit randomly in the gallaxy. 2. Interstellar Medium: This is the gas and dust that fl ...
... (c) Halo: The halo contains only older stars, almost all inside the globular clusters also found there. There is no gas and dust, and what stars are there have very low concentrations of heavy elements. They also orbit randomly in the gallaxy. 2. Interstellar Medium: This is the gas and dust that fl ...
Birth and Death of Stars
... • Some massive stars produce leftovers too massive to become stable neutron stars. If the remaining core is > 3 times the mass of the sun, the star may contract further under its greater gravity. The force of contraction crushes the dense core and creates an object so massive and dense that even lig ...
... • Some massive stars produce leftovers too massive to become stable neutron stars. If the remaining core is > 3 times the mass of the sun, the star may contract further under its greater gravity. The force of contraction crushes the dense core and creates an object so massive and dense that even lig ...
The HR Diagram - Faculty Web Pages
... brightnesses. Now let's see if we can find some relationships between these stellar properties. We know that hotter stars are brighter, as described by the Stefan-Boltzmann Law, and we know that the hotter stars are also bluer, as described by Wien's Law. The H-R diagram is a way of displaying an im ...
... brightnesses. Now let's see if we can find some relationships between these stellar properties. We know that hotter stars are brighter, as described by the Stefan-Boltzmann Law, and we know that the hotter stars are also bluer, as described by Wien's Law. The H-R diagram is a way of displaying an im ...
The HR Diagram - Faculty Web Pages
... brightnesses. Now let's see if we can find some relationships between these stellar properties. We know that hotter stars are brighter, as described by the Stefan-Boltzmann Law, and we know that the hotter stars are also bluer, as described by Wien's Law. The H-R diagram is a way of displaying an im ...
... brightnesses. Now let's see if we can find some relationships between these stellar properties. We know that hotter stars are brighter, as described by the Stefan-Boltzmann Law, and we know that the hotter stars are also bluer, as described by Wien's Law. The H-R diagram is a way of displaying an im ...
Measuring Stellar Distances
... To gain a real physical understanding of stars we must determine their intrinsic energy outputs (also known as Luminosity). Think about it for a moment – suppose you had no prior knowledge of what stars actually were – that you lived in a time where they could be anything. If you simply look up into ...
... To gain a real physical understanding of stars we must determine their intrinsic energy outputs (also known as Luminosity). Think about it for a moment – suppose you had no prior knowledge of what stars actually were – that you lived in a time where they could be anything. If you simply look up into ...
The birth and life of stars
... The most massive pre–main-sequence stars take the shortest time to become main-sequence stars (O and B stars). In the final stages of pre–main-sequence contraction, when hydrogen fusion is about to begin in the core, the pre–main-sequence star may undergo vigorous chromospheric activity that eje ...
... The most massive pre–main-sequence stars take the shortest time to become main-sequence stars (O and B stars). In the final stages of pre–main-sequence contraction, when hydrogen fusion is about to begin in the core, the pre–main-sequence star may undergo vigorous chromospheric activity that eje ...
neutron star - Livonia Public Schools
... in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. ...
... in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. ...
Lesson 4. Wiens and Stefans Laws
... 1. The peak intensity of thermal radiation from the Sun is at a wavelength of 500 nm, calculate the surface temperature of the Sun. 2. A star has a power output of 6.0 x 1028 W and a surface temperature of 3400K, calculate its radius and the ratio to the Sun’s radius (rsun = 7 x 108 m) ...
... 1. The peak intensity of thermal radiation from the Sun is at a wavelength of 500 nm, calculate the surface temperature of the Sun. 2. A star has a power output of 6.0 x 1028 W and a surface temperature of 3400K, calculate its radius and the ratio to the Sun’s radius (rsun = 7 x 108 m) ...
Document
... degenerate until the final burning stages. The core at that point consists of iron. Other elements – hydrogen, helium, carbon, oxygen, and silicon, burn in successive layers (moving inward). The luminosity is almost constant, at all stages of the evolution. These stars move horizontally across the H ...
... degenerate until the final burning stages. The core at that point consists of iron. Other elements – hydrogen, helium, carbon, oxygen, and silicon, burn in successive layers (moving inward). The luminosity is almost constant, at all stages of the evolution. These stars move horizontally across the H ...
Giant Stars
... The Future Sun • The Sun will spend about 10 billion years on the main sequence. ...
... The Future Sun • The Sun will spend about 10 billion years on the main sequence. ...
five minute episode script
... DISTINCTIVE BELT OF THREE STARS. IF YOU LOOK A LITTLE CLOSER YOU'LL SEE STARS OF DIFFERENT BRIGHTNESS AND COLOR. DEAN: STAR COLOR IS AN INDICATION OF ITS TEMPERATURE - BLUE STARS BEING THE HOTTEST AND RED STARS BEING THE COLDEST. YOU CAN REALLY SEE THE COLORS OF THE BRIGHTEST STARS LIKE THOSE IN ORI ...
... DISTINCTIVE BELT OF THREE STARS. IF YOU LOOK A LITTLE CLOSER YOU'LL SEE STARS OF DIFFERENT BRIGHTNESS AND COLOR. DEAN: STAR COLOR IS AN INDICATION OF ITS TEMPERATURE - BLUE STARS BEING THE HOTTEST AND RED STARS BEING THE COLDEST. YOU CAN REALLY SEE THE COLORS OF THE BRIGHTEST STARS LIKE THOSE IN ORI ...
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.