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Astronomy: explore STEM content (page 19 of 26) · openstem
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Astronomy
Stars, orbits, cosmology and observation on openstem — flashcards, notes, quizzes and plots shared by the community. Study free, or clone anything into your library.
Almost entirely neutrons, packed together at nuclear densities — the collapsed core of a massive star, left over after a supernova, supported against further collapse by neutron degeneracy pressure.
What causes relativistic beaming of a jet's radiation?
AGravitational lensing by the central black holeBRelativistic aberration sweeping emission forward into a narrow cone around the direction of motionCMagnetic reflection off the accretion diskDScattering of the jet's own radiation by interstellar dust
Why are binary star systems so important for measuring stellar masses?1 / 8
Mass cannot be measured directly from a star's light — only its effects on motion reveal it. In a binary system, the two stars' mutual gravitational orbit obeys Kepler's laws in a form that depends on both masses, so measuring the orbit (period and separation) directly yields the total system mass — binaries are essentially the only way to measure stellar masses independently of stellar models.
Astronomy
Astronomy · L4 · Binary Star Systems & the Mass-Period Relation
A Rivalry Reaches Orbit In the years after World War II, the United States and the Soviet Union became rival superpowers locked in the Cold War. Beyond weapons and politics, the two nations competed to prove technological superiority — and
What is a primordial black hole (PBH), and how does its formation differ from a stellar-collapse black hole?1 / 7
A primordial black hole forms not from the collapse of a dying star, but from the direct gravitational collapse of an unusually large density perturbation in the very early universe, at the moment that perturbation's scale re-enters the causal horizon. Because they don't require a stellar progenitor, PBHs could in principle span an enormous mass range — from far below a solar mass up to, speculatively, supermassive scales.
Stellar structure: hydrostatic equilibrium and mass continuity A star is a self-gravitating ball of hot plasma held in a delicate, long-lived balance. The basic equations of stellar structure describe that balance at the level of undergradu
Astronomy
Astronomy · L4 · Stellar structure: hydrostatic equilibrium and mass continuity
What is a blackbody, and why are stars well approximated as blackbodies?1 / 8
A blackbody is an idealised object that absorbs all incident radiation (reflecting none) and re-emits energy purely as a function of its temperature, with a specific, universal spectral shape (the Planck spectrum). Stellar photospheres are dense, opaque plasma that absorb and re-emit radiation many times before it escapes, closely approximating this idealised thermal equilibrium — so stars' continuous spectra are well fit by blackbody curves.
Astronomy
Astronomy · L4 · Blackbody Radiation & the Luminosity-Radius-Temperature Relation
Same Material, Different Light A nebula is, at its simplest, an interstellar cloud of gas and dust. What separates the different named types is not what the cloud is made of, but how — or whether — it produces visible light, which in turn d
The Outer Edge of the Solar System Beyond Jupiter and Saturn lie two more giant planets: Uranus and Neptune. They are farther from the Sun, colder, and smaller than Jupiter and Saturn, but they are still much bigger than Earth. Because they
Astronomy
Astronomy · L1 · Neptune and Uranus, the Ice Giants
AWind blowing across the ocean surfaceBThe Moon's gravity pulling on Earth's oceansCEarth's rotation alone, with no outside influenceDOcean currents changing temperature