how is our Sun dying...?

Answer 1

Our sun is in it's "Main Sequence" and is not due to run out of fuel for approximately five billion years. It is about halfway through it's main sequence life, so it's probably overstating the case to say that it is dying. It is a relatively small star, so it's lifespan is relatively long. A star's size and it's longevity are conversely related.

Jenrules13: Dear, shooting stars are NOT dying stars!!! They are small mineral fragments entering our atmosphere at high velocity. The Sun WILL NOT die in a few million years (as far as we know). Please take a science class.

OceanSylvinia: No, our sun will not become a black hole. That fate is reserved for stars far more massive then our own. It also will not go nova or supernova. It's much too small.

Answer 2

well when our star does finally die 1of 2 things Will happen firstly our sun Will turn into a red giant and explode and mercury Venus earth and mars will also go with the giant or the sun will turn into a white dwarf and stay like that for a while giving of a little heat so only the toughest species will survive but not 4 long the dwarf will keep getting smaller and more density and turn in to a black hole but that's not if the black hole at the end of our universe gets us first but that wont happen 4 a very long time

Answer 3

Technically our sun isn't "dying" right now. Its total liftetime should be some 10-billion years, and currently it's 4.5- to 5-billion years old. It's only in middle age and quite stable. In about 4-billion years or so it will begin dying as it starts running out of fuel for the nuclear fusion process that takes place in its core. Eventually it will swell into a red-giant star, then slowly grow cooler and cooler and shrink down to an object about the same diameter as Earth. At that time it will be a white-dwarf star, virtually dead.

Answer 4

A dying sun blows off a shell of gas, it expands to more than 50 times its original size and eventually blows out. Would you like to see some interesting pictures painted by gases taken by the Hubble? This is the last days of a star, but also a picture, story found in REVELATION. Read and click

Answer 5

It isn't really dying. But it is using up its hydrogen fuel, which is not being replenished. In billions of years it will run out. Nothing lasts forever, but to a person who only lives 100 years, or even all recorded history (which is only a few thousand years), billions of years is effectively forever.

Answer 6

It undergoing a continuous fusion reaction to produce it's energy output.

The reaction is hydrogen atoms are fused to helium atoms and an emission of electromagnetic energy on a wide range of frequencies.

Answer 7

Sun is a star and all star cycle end up die but it only happened in very long time, we still have time...
until it used up it fuel to produce the burning reaction, give us light.
after that, I don't know

Answer 8

you shouldn't worry about that ... that will happen in several thousand years ahead ...
the basics of that are that like a burning piece of wood...our sun little by little is burning itself ....
but for now our attention might as well be the temperature here mainly at the poles ........

Answer 9

Our Sun is a normal main-sequence G2 star, one of more than 100 billion stars in our galaxy.

diameter: 1,390,000 km.
mass: 1.989e30 kg
temperature: 5800 K (surface)
15,600,000 K (core)

The Sun is by far the largest object in the solar system. It contains more than 99.8% of the total mass of the Solar System (Jupiter contains most of the rest).

It is often said that the Sun is an "ordinary" star. That's true in the sense that there are many others similar to it. But there are many more smaller stars than larger ones; the Sun is in the top 10% by mass. The median size of stars in our galaxy is probably less than half the mass of the Sun.

The Sun is personified in many mythologies: the Greeks called it Helios and the Romans called it Sol.

The Sun is, at present, about 70% hydrogen and 28% helium by mass everything else ("metals") amounts to less than 2%. This changes slowly over time as the Sun converts hydrogen to helium in its core.

The outer layers of the Sun exhibit differential rotation: at the equator the surface rotates once every 25.4 days; near the poles it's as much as 36 days. This odd behavior is due to the fact that the Sun is not a solid body like the Earth. Similar effects are seen in the gas planets. The differential rotation extends considerably down into the interior of the Sun but the core of the Sun rotates as a solid body.

Conditions at the Sun's core (approximately the inner 25% of its radius) are extreme. The temperature is 15.6 million Kelvin and the pressure is 250 billion atmospheres. At the center of the core the Sun's density is more than 150 times that of water.

The Sun's energy output (3.86e33 ergs/second or 386 billion billion megawatts) is produced by nuclear fusion reactions. Each second about 700,000,000 tons of hydrogen are converted to about 695,000,000 tons of helium and 5,000,000 tons (=3.86e33 ergs) of energy in the form of gamma rays. As it travels out toward the surface, the energy is continuously absorbed and re-emitted at lower and lower temperatures so that by the time it reaches the surface, it is primarily visible light. For the last 20% of the way to the surface the energy is carried more by convection than by radiation.

The surface of the Sun, called the photosphere, is at a temperature of about 5800 K. Sunspots are "cool" regions, only 3800 K (they look dark only by comparison with the surrounding regions). Sunspots can be very large, as much as 50,000 km in diameter. Sunspots are caused by complicated and not very well understood interactions with the Sun's magnetic field.

A small region known as the chromosphere lies above the photosphere.

The highly rarefied region above the chromosphere, called the corona, extends millions of kilometers into space but is visible only during a total solar eclipse (left). Temperatures in the corona are over 1,000,000 K.

It just happens that the Moon and the Sun appear the same size in the sky as viewed from the Earth. And since the Moon orbits the Earth in approximately the same plane as the Earth's orbit around the Sun sometimes the Moon comes directly between the Earth and the Sun. This is called a solar eclipse; if the alignment is slighly imperfect then the Moon covers only part of the Sun's disk and the event is called a partial eclipse. When it lines up perfectly the entire solar disk is blocked and it is called a total eclipse of the Sun. Partial eclipses are visible over a wide area of the Earth but the region from which a total eclipse is visible, called the path of totality, is very narrow, just a few kilometers (though it is usually thousands of kilometers long). Eclipses of the Sun happen once or twice a year. If you stay home, you're likely to see a partial eclipse several times per decade. But since the path of totality is so small it is very unlikely that it will cross you home. So people often travel half way around the world just to see a total solar eclipse. To stand in the shadow of the Moon is an awesome experience. For a few precious minutes it gets dark in the middle of the day. The stars come out. The animals and birds think it's time to sleep. And you can see the solar corona. It is well worth a major journey.

The Sun's magnetic field is very strong (by terrestrial standards) and very complicated. Its magnetosphere (also known as the heliosphere) extends well beyond Pluto.

In addition to heat and light, the Sun also emits a low density stream of charged particles (mostly electrons and protons) known as the solar wind which propagates throughout the solar system at about 450 km/sec. The solar wind and the much higher energy particles ejected by solar flares can have dramatic effects on the Earth ranging from power line surges to radio interference to the beautiful aurora borealis.

Recent data from the spacecraft Ulysses show that during the minimum of the solar cycle the solar wind emanating from the polar regions flows at nearly double the rate, 750 kilometers per second, that it does at lower latitudes. The composition of the solar wind also appears to differ in the polar regions. During the solar maximum, however, the solar wind moves at an intermediate speed.

Further study of the solar wind will be done by the recently launched Wind, ACE and SOHO spacecraft from the dynamically stable vantage point directly between the Earth and the Sun about 1.6 million km from Earth.

The solar wind has large effects on the tails of comets and even has measurable effects on the trajectories of spacecraft.

Spectacular loops and prominences are often visible on the Sun's limb (left).

The Sun's output is not entirely constant. Nor is the amount of sunspot activity. There was a period of very low sunspot activity in the latter half of the 17th century called the Maunder Minimum. It coincides with an abnormally cold period in northern Europe sometimes known as the Little Ice Age. Since the formation of the solar system the Sun's output has increased by about 40%.

The Sun is about 4.5 billion years old. Since its birth it has used up about half of the hydrogen in its core. It will continue to radiate "peacefully" for another 5 billion years or so (although its luminosity will approximately double in that time). But eventually it will run out of hydrogen fuel. It will then be forced into radical changes which, though commonplace by stellar standards, will result in the total destruction of the Earth (and probably the creation of a planetary nebula).

Answer 10

It is running out of fuel - don't worry it won't happen for a billion or so years.