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What else can I help you with?
What are the parts of the sun and their function?
The PhotosphereThe Sun has basically the same chemicalelements as found on Earth. However, the Sun is so hot that all of these elements exist in the gaseous state. There is not really a "surface" to the Sun. Think of it this way: the Sun is a bunch of gas which gets denser and denser as you move from space toward the solar core. The photosphere would then represent the depth at which we can see no deeper toward the core. Think of what a thick cloud looks like when you look down on it from an airplane - it looks solid, but it isn't.The Parts of a StarThe Sun's atmosphere changes from being transparent to being opaque over a distance of only a few hundred kilometers. This is remarkable given the size of the Sun, and represents such a huge change that we often think of it as a true boundary. When we speak of the size of the Sun, we usually mean the size of the region surrounded by the photosphere. The photosphere is slightly different from one place on the Sun to another, but in general is has a pressure about a few hundredths of the sea-level pressure on Earth, a density of about a ten-thousandth of the Earth's sea-level atmospheric density, and a temperature in the range 4500-6000 Kelvin.The ChromosphereThe gases which extend away from the photosphere make up the chromosphere. These gases are transparent to most visible radiation. The chromosphere is about 2500 km thick. The density of the gases decreases as you move away from the photosphere into the chromosphere, but the temperature increases! From the bottom to the top of the chromosphere, the average temperature goes from 4500 to 10,000 Kelvin! Needless to say, this rise was not anticipated by scientists when they first measured it. Throughout the rest of the Sun, temperature decreases as you move further away from the core. The Solar Corona seen duringa total eclipseThe CoronaThe chromosphere merges into the outermost region of the Sun's atmosphere, the corona. The corona extends for millions of miles into space above the photosphere. Usually, we cannot see the corona because of the brightness of the photosphere. However, during a total solar eclipse, the corona shines beautifully against the dark sky. The corona has a density about 0.0000000001 times that of the Earth's sea-level atmosphere. It is very hot - millions of Kelvin. Because of this high temperature, the bulk of the radiation from the corona is emitted atultraviolet and X-ray wavelengths. Magnetic fields on the Sun seem to play an important part in heating the gas to such a high temperature. However, the exact way that this happens is not well understood. The image you see to the left was taken during a solar eclipse in 1980; lightfrom the photosphere is blocked out by the Moon (the dark disk). A Few Other Solar FeaturesThe Solar WindThe solar wind is nothing more than a stream of charged particles flowing outward from the Sun with an average velocity of about 400 km/sec. It is a natural consequence of the Sun being so hot - the corona gas has too much energy to be gravitationally bound to the Sun. Sunspots and Their CycleSunspots are cooler regions on the Sun's photosphere (about 1500 K cooler) and so appear to be darker than the photosphere. A given sunspot can have a lifetime ranging from a few hours to a few months. It consists of two parts - the dark inside region called the umbra and the surrounding less dark region called the penumbra. Their sizes vary over a wide range, with a few having been measured to be 50,000 km in diameter! A German amateur astronomer, Heinrich Schwabe, published a paper in 1851 which stated that the number of sunspots visible on average varied with a period of about 10 years. This conclusion has been substantiated by observations over the 140 years since. The period of repetition on average is 11.1 years, but has been as short as 8 years and as long as 16 years.
Describe in general the structure and interior density pressure and temperature conditions of an average star such as the Sun?
The interior of an average star is modeled after the theoretical pressure, temperature, and density conditions that would be necessary to produce the observed energy and light from the surface. The interior can be described as (1) the core, (2) a radiation zone, and (3) the convection zone. The core is a dense and very hot region where the density fo the core is about 12 times that of solid lead. The radiation zone is less dense and energy in the form of gamma and x rays from the core is absorbed and reemitted by collisions with atoms in this zone. The convection zone begins about seven-tenths of the way to the surface, where the density of the gases is about 1% of the density of water. Gases at the bottom of this zone are heated by radiation from the radiation zone below, expand from heating, and rise to the surface by convection.
How does temperature change as altitude increases through all layers of the atmosphere?
In the troposphere, the temperature generally decreases with increasing altitude due to lower air pressure. In the stratosphere, the temperature remains relatively constant then begins to increase due to the absorption of solar radiation by ozone. In the mesosphere and thermosphere, the temperature decreases again as altitude increases due to a decrease in the density of air molecules.
What is the general relationship between temperature and distance from the sun?
The general relationship between temperature and distance from the sun is that temperature decreases as distance from the sun increases. This is because the sun is the primary source of heat in our solar system, and objects farther from the sun receive less solar energy and are therefore colder.
What is a stars internal temperature?
A star's internal temperature can vary depending on its size and age, but in general, the core temperature of a star like our sun is around 15 million degrees Celsius. This high temperature is necessary for nuclear fusion to occur and sustain the star's energy production.
What are the parts of the sun and their function?
The PhotosphereThe Sun has basically the same chemicalelements as found on Earth. However, the Sun is so hot that all of these elements exist in the gaseous state. There is not really a "surface" to the Sun. Think of it this way: the Sun is a bunch of gas which gets denser and denser as you move from space toward the solar core. The photosphere would then represent the depth at which we can see no deeper toward the core. Think of what a thick cloud looks like when you look down on it from an airplane - it looks solid, but it isn't.The Parts of a StarThe Sun's atmosphere changes from being transparent to being opaque over a distance of only a few hundred kilometers. This is remarkable given the size of the Sun, and represents such a huge change that we often think of it as a true boundary. When we speak of the size of the Sun, we usually mean the size of the region surrounded by the photosphere. The photosphere is slightly different from one place on the Sun to another, but in general is has a pressure about a few hundredths of the sea-level pressure on Earth, a density of about a ten-thousandth of the Earth's sea-level atmospheric density, and a temperature in the range 4500-6000 Kelvin.The ChromosphereThe gases which extend away from the photosphere make up the chromosphere. These gases are transparent to most visible radiation. The chromosphere is about 2500 km thick. The density of the gases decreases as you move away from the photosphere into the chromosphere, but the temperature increases! From the bottom to the top of the chromosphere, the average temperature goes from 4500 to 10,000 Kelvin! Needless to say, this rise was not anticipated by scientists when they first measured it. Throughout the rest of the Sun, temperature decreases as you move further away from the core. The Solar Corona seen duringa total eclipseThe CoronaThe chromosphere merges into the outermost region of the Sun's atmosphere, the corona. The corona extends for millions of miles into space above the photosphere. Usually, we cannot see the corona because of the brightness of the photosphere. However, during a total solar eclipse, the corona shines beautifully against the dark sky. The corona has a density about 0.0000000001 times that of the Earth's sea-level atmosphere. It is very hot - millions of Kelvin. Because of this high temperature, the bulk of the radiation from the corona is emitted atultraviolet and X-ray wavelengths. Magnetic fields on the Sun seem to play an important part in heating the gas to such a high temperature. However, the exact way that this happens is not well understood. The image you see to the left was taken during a solar eclipse in 1980; lightfrom the photosphere is blocked out by the Moon (the dark disk). A Few Other Solar FeaturesThe Solar WindThe solar wind is nothing more than a stream of charged particles flowing outward from the Sun with an average velocity of about 400 km/sec. It is a natural consequence of the Sun being so hot - the corona gas has too much energy to be gravitationally bound to the Sun. Sunspots and Their CycleSunspots are cooler regions on the Sun's photosphere (about 1500 K cooler) and so appear to be darker than the photosphere. A given sunspot can have a lifetime ranging from a few hours to a few months. It consists of two parts - the dark inside region called the umbra and the surrounding less dark region called the penumbra. Their sizes vary over a wide range, with a few having been measured to be 50,000 km in diameter! A German amateur astronomer, Heinrich Schwabe, published a paper in 1851 which stated that the number of sunspots visible on average varied with a period of about 10 years. This conclusion has been substantiated by observations over the 140 years since. The period of repetition on average is 11.1 years, but has been as short as 8 years and as long as 16 years.
In general the density of sea water increases as?
salinity increases and temperature decreases....
Why does density vary with temperature?
In general as things get hotter they expand, and conversely when they cool they contract. This is most noticeable for gases. As the mass remains constant because density is mass/volume as volume increases when temperature goes up the density decreases. The opposite occurs when temperature drops.
10ml is equal to what mg?
That depends on the density of whatever occupies that volume. The general relationship is:mass = density x volumeThat depends on the density of whatever occupies that volume. The general relationship is:mass = density x volumeThat depends on the density of whatever occupies that volume. The general relationship is:mass = density x volumeThat depends on the density of whatever occupies that volume. The general relationship is:mass = density x volume
Temp. of SUN?
For sure I don't know the general temperature of the sun. The sun's surface, also known as the photosphere is about 5,500 degrees Celsius. The sun's core is about fifteen million degrees Celsius. There are other parts like the radiation zone and the convection zone, but I do not know the temperature for the other parts. Hope this was use full information to you.
What is the population density of General Carneiro?
General Carneiro's population density is 14.8 people per square kilometer.
What two factors effect the speed of sound?
The two main factors that affect the speed of sound in a material are the density of the material and the elasticity of the material. In general, sound travels faster in materials that are more dense and have higher elasticity.
How do you determine the density?
Density in general is found by Mass divided by the volume
What is the population density of General Isidoro Resquín?
General Isidoro Resquín's population density is 57.48 people per square kilometer.
What is the density of furnace oil at 120 degree c?
The density of furnace oil at 120 degrees Celsius may vary depending on the specific composition of the oil. However, as a general estimate, the density of furnace oil at this temperature is typically around 0.9 - 0.95 grams per cubic centimeter.
In general an increase in temperature?
A general increase in temperature increases the reaction rate.
Why does the density of a substance change with temperature?
As the temperature increases, the molecules gain more energy, and they move faster. As a consequence, they tend to move farther apart from each other thus taking up more space/volume. Density is the mass/volume. Since the mass does not change, and the volume increases, the density, in general, will decrease with increasing temperature.
