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11 maj 2023 · The temperature of the sun varies from around 27 million degrees Fahrenheit (15 million degrees Celsius) at the core to only about 10,000 degrees F (5,500 degrees C) at the surface, according...
- Curious Kids
The temperature of the sun. Heat is created in the very...
- Hydrogen and Helium
In the sun's core, gravitational forces create tremendous...
- How Was the Sun Formed
The Sun: Our Perfectly Average Middle Aged Star (Image...
- When Will the Sun Die
That's when the sun will become a red giant, which it will...
- Parker Solar Probe
NASA's Parker Solar Probe is on a mission to study the sun...
- Gravity
Gravity can be described in a variety of ways. Here's how...
- NASA's Lucy Asteroid-Hopping Probe Captures 1st Snapshot of Space Rock 'Dinky' (Photo)
NASA's Lucy spacecraft just sent home an impressive glimpse...
- James Webb Space Telescope Deepens Major Debate Over Universe's Expansion Rate
According to most models, the Hubble constant should equal...
- Curious Kids
13 gru 2023 · The photosphere is the visible surface of the Sun. Temperature: Roughly 5,500 K. In Celsius: About 5,300 °C (usually rounded up to 5.500 °C) In Fahrenheit: Approximately 9,500 °F (usually rounded up to 10,000 °F) This layer emits the light we see, appearing bright due to the contrast with cooler outer layers.
How do we know the temperature at the centre of the Sun? - BBC Science Focus Magazine.
22 wrz 2022 · The temperature at the very center of the Sun is about 15,000,000° C (27,000,000° F) and the density is about 150 g/cm³ (approximately 10 times the density of gold, 19.3 g/cm³ or lead, 11.3 g/cm³). Both the temperature and the density decrease as one moves outward from the center of the Sun.
The luminosity stays approximately constant as the temperature increases, with the ejected half of the Sun's mass becoming ionized into a planetary nebula as the exposed core reaches 30,000 K (53,500 °F), as if it is in a sort of blue loop.
The temperature in the Sun's core is about 27 million degrees Fahrenheit (15 million degrees Celsius) – hot enough to sustain nuclear fusion. This creates outward pressure that supports the star's gigantic mass, keeping it from collapsing.
• Both the “approximate” temperature structure, and the “detailed” temperature structure, hold fascinating solar science questions (e.g coronal heating; prominence formation, stability, and instability). 50
