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Scales that defeat intuition

Distances, times and densities so far outside experience that the only reliable instrument is arithmetic.
common periapsiscircleellipse, e = 0.5ellipse, e = 0.9parabola, e = 1hyperbola, e = 1.5e < 1 returnse ≥ 1 never does Orbits

Every orbit one force allows, and the number that picks between them

Circle, ellipse, parabola, hyperbola. A single inverse-square force permits exactly these four, and one number decides which — including whether the body ever comes back.

celestial poleobserverzenithnorthsouthcelestial equatorthe daily circle of a star at δ = 20°the pole sits 52° up, because the observer is at latitude 52°faint arcs are below the horizon The observed sky

The sphere that is not there, and why it is still the right model

The stars are at wildly different distances and the celestial sphere is a fiction. It is also the most useful fiction in observational astronomy, because for pointing at things, distance is exactly the information to throw away.

distant starsJanuaryJuly2 AU1.3 pc2p = 1.54″distance = 1 ÷ parallax in arcsecondsangles hugely exaggerated: the true angle here is a five-thousandth of a degree Starlight

The triangle that reaches the stars, and stops

Parallax is the only distance measurement in astronomy that assumes nothing. It is also the only one with a hard ceiling, and everything beyond that ceiling rests on it.

R = 0.01R☉R = 0.1R☉R = R☉R = 10R☉R = 100R☉giantssupergiantswhite dwarfs1M☉3M☉20M☉40M☉the Sun10−410−21102104106surface temperature (K), increasing to the leftluminosity, in solar units Stars

The diagram that sorted the stars, by plotting two things against each other

Plot brightness against colour for a few thousand stars and they do not scatter. They fall on a narrow band with two islands off it, and explaining that structure is most of stellar astronomy.

0.100.321.03.210320.011.0100100001000000mass (solar units)0.2M☉ → 0.01L☉1M☉ → 1L☉5M☉ → 391L☉20M☉ → 50,088L☉dashed: a pure slope of 3.5 Stars

Mass decides everything, by a power of three and a half

Two stars of the same mass are almost the same star. Double the mass and the output multiplies by eleven — which is why a modest range of masses produces a colossal range of stars.

0.321.03.2103210^610^710^810^910^1010^1110^12mass (solar units)the age of the universe0.5M☉ — 80 Gyr1M☉ — 10 Gyr3M☉ — 458 Myr10M☉ — 23 Myr30M☉ — 1 Myrslope ≈ −2.5 Stars

Why the biggest stars die first, and take the galaxy with them

A star thirty times the Sun's mass has thirty times the fuel and burns it forty thousand times faster. It lasts a few million years, and everything heavier than iron exists because of it.

2468101200.511.5distance, in body radiiescape speedcircular speedthe surfacea high orbitgeostationarythe gap is always a factor of √2 Spaceflight

The speed that does not come back, and the √2 that separates it

Escape speed is exactly the square root of two times circular speed, at every distance from every body. Being in orbit is already 71% of the way to leaving.

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