Density of the sun

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Density of the Sun: An In-Depth Analysis

Average Density of the Sun

The Sun, a massive sphere of hot gaseous matter, has an average density of approximately 1.4 g/cm³. This value is derived from its mass, which is about (2 \times 10^{33}) grams, and its radius, which is around (7 \times 10^5) kilometers . The density varies significantly from the core to the outer layers.

Core Density and Temperature

At the core of the Sun, where nuclear fusion occurs, the density is extremely high, approximately 160 times the density of water. This core region, which constitutes about 10% of the Sun's mass, has a temperature of around 16 million Kelvin . The intense gravitational compression from the layers above contributes to this high density and temperature.

Density Gradient from Core to Photosphere

The density of the Sun decreases dramatically from the core to the outer layers. At the solar center, the density is about 70 g/cm³, but it drops to around (10^{-7}) g/cm³ in the photosphere, the Sun's visible surface . This gradient is a result of the decreasing pressure and temperature as one moves outward from the core.

Solar Corona and Electron Density

The solar corona, the outermost part of the Sun's atmosphere, also exhibits a specific density structure. The electron density in the corona has been quantitatively described, with early studies by Baumbach and later improvements by Allen and van de Hulst, leading to the well-known Allen-Baumbach relation . This relation helps in understanding the scattering of white light by free electrons in the corona.

Radial Evolution of Density in the Solar Corona

Observations from instruments like the SOHO coronagraphs and the HAO Mauna Loa Mk III K-coronameter have shown that the density structure in the solar corona evolves radially. The density gradient observed close to the Sun at 1.15 solar radii is carried into interplanetary space, maintaining a similar gradient, except in the case of coronal streamers .

Conclusion

The Sun's density varies significantly from its core to its outer layers, with the core being extremely dense and hot due to gravitational compression. The density decreases outward, reaching very low values in the photosphere and the corona. Understanding these density variations is crucial for comprehending the Sun's structure and the dynamics of its atmosphere.

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Most relevant research papers on this topic

The dark matter density at the Sun’s location

The dark matter density at the Sun's location is 0:43(11)(10) GeV/cm3 using the local equation of centrifugal equilibrium, with uncertainties due to the slope of the circular-velocity at the Sun location and the ratio between this radius and the stellar exponential thin disk length scale.

Highly Cited

2010·

364citations

·P. Salucci et al.

Radial evolution of density structure in the solar corona

The solar corona's density structure, influenced by coronal streamers, radially evolves into interplanetary space with the same density gradient, except for coronal streamers that evolve into the heliospheric current sheet.

1999·

23citations

·R. Woo et al.

The Solar Photosphere

The solar photosphere has a density of 10-7 gem-3, which is significantly lower than the solar center's 70 gem-3 density, and is a temperature of 14 106 °K.

1965·

3citations

·C. Jager

Solar Radiation Models and Information for Renewable Energy Applications

The Sun's core temperature is about 16 million K and has a density of about 160 times the density of water, making it very hot and dense.

2012·

6citations

·E. Falayi et al.

Seasonal variations of thermospheric mass density at dawn/dusk from GOCE observations

Seasonal variations in thermospheric mass density show hemispheric asymmetry, with large amplitudes in the Southern Hemisphere, strong latitudinal and solar activity dependences, and varying effects of latitude and solar activity.

2018·

12citations

·L. Weng et al.

The Density and Depth of the Solar Atmosphere

The solar atmosphere's density and depth are determined by the temperature and pressure of the solar surface, not the volume of the terrestrial atmosphere.

1871·

14citations

·Thule

Density of Neutral Hydrogen in the Sun's Interstellar Neighborhood

The interstellar neutral hydrogen density is 40% higher than previously thought, suggesting higher charge exchange rates at the heliospheric boundaries and a less asymmetric shape of the heliosphere.

2020·

61citations

·P. Swaczyna et al.

ELECTRON DENSITY IN THE SOLAR CORONA

Baumbach's method, using brightness distribution in the corona during solar eclipses, provided an average electron density profile for the solar corona.

Highly Cited

1966·

73citations

·J. Harrington

Kilometre-scale structures in the Sun's corona

The Sun's corona contains kilometre-scale filamentary structures, which transition from rotating structures to turbulent density irregularities convecting with the solar wind.

1996·

49citations

·R. Woo

Atomic and Radiative Processes in the Solar Interior

The Sun's high density and temperature, along with its high central pressure, prevent it from collapsing.

1986·

29citations

·W. Huebner

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