STARS
... The greater a stars mass, the greater is the amount of its nuclear fuel. However, the more massive stars are fuel guzzlers. They shine much brighter than less massive stars and use up their fuel very fast. So the more massive stars have shorter lives. Our sun will last about 10 billion years ( we a ...
... The greater a stars mass, the greater is the amount of its nuclear fuel. However, the more massive stars are fuel guzzlers. They shine much brighter than less massive stars and use up their fuel very fast. So the more massive stars have shorter lives. Our sun will last about 10 billion years ( we a ...
Homework #2
... b) Suppose another Cepheid also with m = 20.0 had that same period, but was actually Type II and thus had an absolute magnitude 1.5 magnitudes larger (i.e., 1.5 added to its magnitude making it a larger number and therefore fainter) than plotted here, [or alternatively the diagram had been miscalibr ...
... b) Suppose another Cepheid also with m = 20.0 had that same period, but was actually Type II and thus had an absolute magnitude 1.5 magnitudes larger (i.e., 1.5 added to its magnitude making it a larger number and therefore fainter) than plotted here, [or alternatively the diagram had been miscalibr ...
Stars
... From this point on, the core cools down like an ordinary object. While it is still hot enough to be seen, such a core is known as a white dwarf star. Compared to other stars, white dwarfs are tiny. More remarkable is the way that the radius of a white dwarf depends on its mass. In normal main sequen ...
... From this point on, the core cools down like an ordinary object. While it is still hot enough to be seen, such a core is known as a white dwarf star. Compared to other stars, white dwarfs are tiny. More remarkable is the way that the radius of a white dwarf depends on its mass. In normal main sequen ...
Activity 10: Lifecycle Of A Star
... 5. What happens after this point depends on the _______ of the star. A star the size of our ...
... 5. What happens after this point depends on the _______ of the star. A star the size of our ...
Outline2a
... Star Forming Regions in the Infrared Due to the friction in the disk, matter flows onto the star. As the star’s mass increases, its core grows hotter. At this time, since the star is still surrounded by dust, it is invisible in the optical. But the heat from the star begins to warm the dust. ...
... Star Forming Regions in the Infrared Due to the friction in the disk, matter flows onto the star. As the star’s mass increases, its core grows hotter. At this time, since the star is still surrounded by dust, it is invisible in the optical. But the heat from the star begins to warm the dust. ...
Life and Evolution of a Massive Star
... the gravitational well where vesc = c 2GM M Rs 2 3.0 km c M Sun ...
... the gravitational well where vesc = c 2GM M Rs 2 3.0 km c M Sun ...
answers2004_05_BC - Particle Physics and Particle Astrophysics
... almost all systems have only one giant planet, and very few indeed have more than 2 (cf. Jupiter and much smaller Saturn in solar system) planets are discovered around stars with heavy element content similar to or higher than the Sun spectral class is also similar to the Sun’s ...
... almost all systems have only one giant planet, and very few indeed have more than 2 (cf. Jupiter and much smaller Saturn in solar system) planets are discovered around stars with heavy element content similar to or higher than the Sun spectral class is also similar to the Sun’s ...
Spectroscopy – the study of the colors of light (the spectrum) given
... spectroscopic parallax to distinguish between red giants and red dwarfs and between white dwarfs and white giants. Therefore the distance to the other 10% of stars not on the main sequence can be found. ...
... spectroscopic parallax to distinguish between red giants and red dwarfs and between white dwarfs and white giants. Therefore the distance to the other 10% of stars not on the main sequence can be found. ...
1 WHY DO THE STARS IN ORION LOOK SO DIFFERENT FROM
... Luminosity shows the relationship of stars’ radii and surface temperature. Each of the stars in Table 1 is many times more luminous than our sun, and emits enormous amounts of energy. Luminosity is related to a stars surface area and temperature. Two stars having the same temperature and size will b ...
... Luminosity shows the relationship of stars’ radii and surface temperature. Each of the stars in Table 1 is many times more luminous than our sun, and emits enormous amounts of energy. Luminosity is related to a stars surface area and temperature. Two stars having the same temperature and size will b ...
stellar_explosions - UT Austin (Astronomy)
... (more massive) a black hole. Let’s see how this occurs. (Remember, this is all theoretical calculations, but later you’ll see that there is surprising observational confirmation for these calculations.) Core is layered like an onion, with heavier elements closer to center (since they are the ashes o ...
... (more massive) a black hole. Let’s see how this occurs. (Remember, this is all theoretical calculations, but later you’ll see that there is surprising observational confirmation for these calculations.) Core is layered like an onion, with heavier elements closer to center (since they are the ashes o ...
PHY111 Stellar Evolution
... luminosity as they evolve, but do change in colour (so they must change in size) ...
... luminosity as they evolve, but do change in colour (so they must change in size) ...
Stars: from Adolescence to Old Age
... – pressure due to fusion in core • hydrogen in the core eventually converted to helium nuclear reactions stop! • gravity takes over and the core shrinks • outside layers also collapse • layers closer to the center collapse faster than those near the surface. • As the layers collapses, the gas comp ...
... – pressure due to fusion in core • hydrogen in the core eventually converted to helium nuclear reactions stop! • gravity takes over and the core shrinks • outside layers also collapse • layers closer to the center collapse faster than those near the surface. • As the layers collapses, the gas comp ...
Name
... 30) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) two helium ...
... 30) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) two helium ...
Name
... 30) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) two helium ...
... 30) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) two helium ...
Name - MIT
... 31) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) three heli ...
... 31) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) three heli ...
Name - MIT
... 31) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) three heli ...
... 31) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) three heli ...
Chap 11 Characterizing Stars v2
... The Hertzsprung-Russell (H-R) diagram is a graph on which luminosities of stars are plotted against their spectral types (or, equivalently, their absolute magnitudes are plotted against surface temperatures). The H-R diagram reveals the existence of four major groupings of stars: main-sequence stars ...
... The Hertzsprung-Russell (H-R) diagram is a graph on which luminosities of stars are plotted against their spectral types (or, equivalently, their absolute magnitudes are plotted against surface temperatures). The H-R diagram reveals the existence of four major groupings of stars: main-sequence stars ...
Shocking Truth about Massive Stars Lidia Oskinova Chandra’s First Decade of Discovery
... fireball.... the inner core of a massive, rapidly rotating star collapses into a ~10 M Kerr black hole ... A superstrong ~10 15 G magnetic field is needed to make the object ... a microquasar. Such events must be vary rare...to account for the ... GRBs’’ ...
... fireball.... the inner core of a massive, rapidly rotating star collapses into a ~10 M Kerr black hole ... A superstrong ~10 15 G magnetic field is needed to make the object ... a microquasar. Such events must be vary rare...to account for the ... GRBs’’ ...
Star
A star is a luminous sphere of plasma held together by its own gravity. The nearest star to Earth is the Sun. Other stars are visible from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, and the brightest stars gained proper names. Extensive catalogues of stars have been assembled by astronomers, which provide standardized star designations.For at least a portion of its life, a star shines due to thermonuclear fusion of hydrogen into helium in its core, releasing energy that traverses the star's interior and then radiates into outer space. Once the hydrogen in the core of a star is nearly exhausted, almost all naturally occurring elements heavier than helium are created by stellar nucleosynthesis during the star's lifetime and, for some stars, by supernova nucleosynthesis when it explodes. Near the end of its life, a star can also contain degenerate matter. Astronomers can determine the mass, age, metallicity (chemical composition), and many other properties of a star by observing its motion through space, luminosity, and spectrum respectively. The total mass of a star is the principal determinant of its evolution and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities, known as a Hertzsprung–Russell diagram (H–R diagram), allows the age and evolutionary state of a star to be determined.A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Once the stellar core is sufficiently dense, hydrogen becomes steadily converted into helium through nuclear fusion, releasing energy in the process. The remainder of the star's interior carries energy away from the core through a combination of radiative and convective processes. The star's internal pressure prevents it from collapsing further under its own gravity. Once the hydrogen fuel at the core is exhausted, a star with at least 0.4 times the mass of the Sun expands to become a red giant, in some cases fusing heavier elements at the core or in shells around the core. The star then evolves into a degenerate form, recycling a portion of its matter into the interstellar environment, where it will contribute to the formation of a new generation of stars with a higher proportion of heavy elements. Meanwhile, the core becomes a stellar remnant: a white dwarf, a neutron star, or (if it is sufficiently massive) a black hole.Binary and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable orbits. When two such stars have a relatively close orbit, their gravitational interaction can have a significant impact on their evolution. Stars can form part of a much larger gravitationally bound structure, such as a star cluster or a galaxy.