• Study Resource
  • Explore
    • Arts & Humanities
    • Business
    • Engineering & Technology
    • Foreign Language
    • History
    • Math
    • Science
    • Social Science

    Top subcategories

    • Advanced Math
    • Algebra
    • Basic Math
    • Calculus
    • Geometry
    • Linear Algebra
    • Pre-Algebra
    • Pre-Calculus
    • Statistics And Probability
    • Trigonometry
    • other →

    Top subcategories

    • Astronomy
    • Astrophysics
    • Biology
    • Chemistry
    • Earth Science
    • Environmental Science
    • Health Science
    • Physics
    • other →

    Top subcategories

    • Anthropology
    • Law
    • Political Science
    • Psychology
    • Sociology
    • other →

    Top subcategories

    • Accounting
    • Economics
    • Finance
    • Management
    • other →

    Top subcategories

    • Aerospace Engineering
    • Bioengineering
    • Chemical Engineering
    • Civil Engineering
    • Computer Science
    • Electrical Engineering
    • Industrial Engineering
    • Mechanical Engineering
    • Web Design
    • other →

    Top subcategories

    • Architecture
    • Communications
    • English
    • Gender Studies
    • Music
    • Performing Arts
    • Philosophy
    • Religious Studies
    • Writing
    • other →

    Top subcategories

    • Ancient History
    • European History
    • US History
    • World History
    • other →

    Top subcategories

    • Croatian
    • Czech
    • Finnish
    • Greek
    • Hindi
    • Japanese
    • Korean
    • Persian
    • Swedish
    • Turkish
    • other →
 
Profile Documents Logout
Upload
How Bright is that Star?
How Bright is that Star?

Conservation of Momentum
Conservation of Momentum

NGC 3370 Spiral Galaxy
NGC 3370 Spiral Galaxy

death_low_mass
death_low_mass

... distance away from us. The apparent brightness is directly related to the star’s luminosity. • Stars in a cluster all have the same chemical abundances. They form from the same cloud so the amount of elements heavier than helium are all the same. • They move together in their orbit, so they all have ...
Lecture 6: Properties of Stars The Constellations The Constellations
Lecture 6: Properties of Stars The Constellations The Constellations

AST121 Introduction to Astronomy
AST121 Introduction to Astronomy

... Binary stars and clusters ...
Stars in Motion
Stars in Motion

Investigate Stars and Galaxies - American Museum of Natural History
Investigate Stars and Galaxies - American Museum of Natural History

AS2001 - University of St Andrews
AS2001 - University of St Andrews

... The quark soup  heavy quark decay Quark-Hadron phase transition and neutron decay  n/p ratio Big Bang nucleosynthesis  primordial abundances Xp = 0.75 ...
IMR_Star Theater
IMR_Star Theater

... If you look at the stars in the night sky long enough, you will notice how groups of stars form familiar objects, something like connect-the-dots pictures. Many centuries ago, people who gazed at the stars noticed pictures out there— and gave names to them. This helped them create a “map” of the nig ...
Lecture 7 February 9
Lecture 7 February 9

... Weak hydrogen lines, strong lines of ionized calcium ...
PPV_hd169142
PPV_hd169142

... accretion rate of 10-8 M yr-1. The available UV data suggest that this material is not reaching the star, and must be being intercepted either by a brown dwarf or planetary mass body. ...
Recurring theme: conservation of energy
Recurring theme: conservation of energy

... Probes knowledge and understanding of the H-R diagram. a)  Draw the H-R diagram, making sure to indicate the axes and the location of the Main Sequence stars [3pt] b) Roughly indicate where is the location of the Sun [1pt] c) Indicate where the hot blue stars are [1 pt] d) Indicate where the cold re ...
Deducing Temperatures and Luminosities of Stars
Deducing Temperatures and Luminosities of Stars

... • EM radiation is the combination of time- and space- varying electric + magnetic fields that convey energy. • Physicists often speak of the “particle-wave duality” of EM ...
Stages 7 to 9 - Sun
Stages 7 to 9 - Sun

Stellar Physics Lecture 1
Stellar Physics Lecture 1

Testing
Testing

... planetary time periods? – Sidereal day (Earth’s rotation with respect to stars) is 4 minutes shorter than a solar day. – Sidereal month (27.3 day orbit of moon) is shorter then synodic month (29.5 day cycle of phases). – Tropical year (cycle of seasons) is 20 minutes shorter than sidereal years (tim ...
New York City Disciple Code - EarthSpaceScience-Keller
New York City Disciple Code - EarthSpaceScience-Keller

... included for most star missing completely Waiter has the ability to know when we want tostages check Most stages include athem Most are missing a description of the description of their core in and when core we want to be left alone. All orders are correct. ...
Time From the Perspective of a Particle Physicist
Time From the Perspective of a Particle Physicist

... • acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e  n + neutrino • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Star or Black Hole • Most SN are this type PHYS 1 ...
star map looking north january-march
star map looking north january-march

... Our nearest large galaxy – Andromeda – can be seen in the Andromeda constellation. It appears to us as an elongated fuzzy blob. The Andromeda galaxy is so far away that its light takes over two million years to reach us. ...
WASP-24b: A New Transiting Close-in Hot Jupiter
WASP-24b: A New Transiting Close-in Hot Jupiter

Star - Uplift Education
Star - Uplift Education

BV Color Index and Temperature - The University of Texas at Dallas
BV Color Index and Temperature - The University of Texas at Dallas

Astronomy 102, Spring 2003 Solutions to Review Problems
Astronomy 102, Spring 2003 Solutions to Review Problems

Acceleration of Coronal Mass Ejection In Long Rising Solar
Acceleration of Coronal Mass Ejection In Long Rising Solar

... The core collapses at the dynamic time scale, i.e. seconds For a core of 1.2 Ms contracting from a density of 109 cm-3 (degenerate electron state, Earth size) to 1015 cm-3 (neutron star, city size), it releases the gravitational energy in the order of 1053 ergs, comparable to the energy released by ...
< 1 ... 55 56 57 58 59 60 61 62 63 ... 167 >

Dyson sphere

A Dyson sphere is a hypothetical megastructure that completely encompasses a star and hence captures most or all of its power output. It was first described by Olaf Stapledon in his science fiction novel, ""Star Maker"". The concept was later popularly adopted by Freeman Dyson. Dyson speculated that such structures would be the logical consequence of the long-term survival and escalating energy needs of a technological civilization, and proposed that searching for evidence of the existence of such structures might lead to the detection of advanced intelligent extraterrestrial life. Different types of Dyson spheres correlate with information on the Kardashev scale.Since then, other variant designs involving building an artificial structure or series of structures to encompass a star have been proposed in exploratory engineering or described in science fiction under the name ""Dyson sphere"". These later proposals have not been limited to solar-power stations. Many involve habitation or industrial elements. Most fictional depictions describe a solid shell of matter enclosing a star, which is considered the least plausible variant of the idea (see below). In May 2013, at the Starship Century Symposium in San Diego, Dyson repeated his comments that he wished the concept had not been named after him.
  • studyres.com © 2025
  • DMCA
  • Privacy
  • Terms
  • Report