Review_game_and_answers
... Each team will discuss and answer each question Scoring sheets are handed in at the end. 5 points to winning team ...
... Each team will discuss and answer each question Scoring sheets are handed in at the end. 5 points to winning team ...
Structure of the Universe
... A ball of gases held together by gravity which produces large amounts of energy. ...
... A ball of gases held together by gravity which produces large amounts of energy. ...
Stars - BrainBytes
... It is estimated there are between 200-400 billion stars in our galaxy The closest star to Earth, besides the sun is Proxima Centauri – located 4.2 light years away ...
... It is estimated there are between 200-400 billion stars in our galaxy The closest star to Earth, besides the sun is Proxima Centauri – located 4.2 light years away ...
Stellar Evolution
... Formation of Stars • Begins with interstellar gas and dust called a nebula • Collapses on self as a result of gravity • Rotates and flattens with hot condensed object at center called a protostar ...
... Formation of Stars • Begins with interstellar gas and dust called a nebula • Collapses on self as a result of gravity • Rotates and flattens with hot condensed object at center called a protostar ...
g9u4c12part3
... star lasts only about 10 billion years. long period of stability expands into a red giant. slowly shrinking into a small, dim white dwarf. it cools into a black dwarf, a dense, dark body made up mostly of carbon and oxygen. ...
... star lasts only about 10 billion years. long period of stability expands into a red giant. slowly shrinking into a small, dim white dwarf. it cools into a black dwarf, a dense, dark body made up mostly of carbon and oxygen. ...
STARS and GALAXIES
... • The sun converts atomic nuclei into energy. • The energy of nuclear fusion of most stars is eventually radiated to space as types of electromagnetic energy. ...
... • The sun converts atomic nuclei into energy. • The energy of nuclear fusion of most stars is eventually radiated to space as types of electromagnetic energy. ...
The Evolutionary Cycle of Stars
... The star eventually converts into a Red Giant & expands to up to 100 times the diameter of the original star. Red Giants develop as the hydrogen in the core is depleted. White Dwarf The final evolutionary state whose mass is not too high. This is the last stage of stellar evolution. ...
... The star eventually converts into a Red Giant & expands to up to 100 times the diameter of the original star. Red Giants develop as the hydrogen in the core is depleted. White Dwarf The final evolutionary state whose mass is not too high. This is the last stage of stellar evolution. ...
Another exAmple: expository mode
... known as nuclear fusion to produce light. As stars use up this hydrogen, in a process that takes billions of years, they pass through certain phases or stages. In each stage, the star’s brightness, temperature, and size change. The redgiant phase occurs when the star begins to run out of hydrogen. I ...
... known as nuclear fusion to produce light. As stars use up this hydrogen, in a process that takes billions of years, they pass through certain phases or stages. In each stage, the star’s brightness, temperature, and size change. The redgiant phase occurs when the star begins to run out of hydrogen. I ...
Stellar Properties and Stellar Evolution Study Guide Name Why
... 5. A shock wave may be the stimulus that causes a nebula to start condensing to form new ...
... 5. A shock wave may be the stimulus that causes a nebula to start condensing to form new ...
Use this form to take notes in class about stars
... Stars of Spectral Classes B to M 9. What color is our sun? ___________what class is it in? ...
... Stars of Spectral Classes B to M 9. What color is our sun? ___________what class is it in? ...
Physical properties of stars
... that are 1,000 times larger than our sun. pg. 450 Temperature: Surface temperatures range from 3000K to 30,000K Color is an indication of temperature. Blue hottest White Yellow Orange Red coolest Mass While the size of stars varies widely the mass does not. 15 times our Sun’s mass to .2 times our Su ...
... that are 1,000 times larger than our sun. pg. 450 Temperature: Surface temperatures range from 3000K to 30,000K Color is an indication of temperature. Blue hottest White Yellow Orange Red coolest Mass While the size of stars varies widely the mass does not. 15 times our Sun’s mass to .2 times our Su ...
22.2 Stars Change Over Their Life Cycles
... Nebula: cloud of gas and dust in which stars may form ...
... Nebula: cloud of gas and dust in which stars may form ...
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.