The Moving Sky: How Star Charts Map a Curved Sky

The moving sky above our head

Above our heads, the dark skies slowly change in appearance. We might think they are eternal and still because the cycle is not apparent to the eye, but in truth they move in an unending rhythm. What we see is not what our great-grandparents saw, and it is definitely not what the ancients saw. Like a top, Earth wobbles on its axis, completing an entire great cycle every 26,000 years. That wobble affects our view of the sky. The wobble is so slow we cannot feel it, but it is wide enough that the pole star changes. Polaris is our pole star now, but for the Egyptians who built the pyramids it was Thuban, and Vega will come after Polaris.

This is why there are two addresses for the stars. Fix your coordinates to the seasons and you get one set. Fix them to the stars themselves and you get another. The gap between them grows by a degree every 72 years. On this page we look at how the poles have wandered, why the zodiac no longer matches the constellations behind it, and how the planets wander against a background that is itself in motion.

The Wandering North Star

Watch the wanderings of the North Star through epochs of time.

The North Star

Why the stars aren’t where your ancestors saw them, the North Star won’t always be north. Earth wobbles, and skies turn.

Sidereal vs. Tropical

Two valid ways to fix a star’s position, one tied to the seasons and one to the stars, and the slowly widening gap between them.

Lahiri Ayanamsa

Modern Indian astronomy needed one exact number to separate the two zodiacs. This is how it was selected

Wandering Planets

The five wandering lights the ancients tracked by eye and how to find tonight’s planets in your own sky.

โœฆ  Astronomy Picture of the Day  โœฆ

Sunspot Stack

April 19, 2001
Credit: SOHO - MDI / EIT Consortiums, Yohkoh / SXT Project
See this entry on NASA's APOD โ†’
Welcome to multiwavelength astronomy ! From top to bottom, these stacked panels show the largest sunspot group in a decade in visible, extreme ultraviolet, and x-ray light. All were taken on March 29, around the time the famous solar active region, cataloged as AR 9393 , was at its peak size -- over 10 times the size of planet Earth. The panels illustrate how the โ€œappearanceโ€ of the active region changes, when imaged in electromagnetic radiation (light) of progressively shorter wavelengths. In the visible light panel, dark islands of sunspots stand out against the bright solar surface, but the situation seems to be reversed in the extreme ultraviolet panel with a bright active region seen against a darker background. Finally, the x-ray panel reveals majestic loops of glowing plasma arcing far above the sunspot group. Why do pictures of the same part of the Sun look so different? Made at different wavelengths, each panel actually records a different layer in the solar atmosphere. Top to bottom, the altitude of each layer (along with temperature) increases; starting with the Sun's visible surface or photosphere (about 5 thousand kelvins), then the chromosphere / transition region (ten to a hundred thousand kelvins ), and finally the solar corona (millions of kelvins).