The apparent aberration of a star is 0 76 arc seconds, and the apparent magnitude is 10 5, how much

To calculate the luminosity of a star, we need to know the mass, volume, and rotation of the star. With this data, we can know the strength of the internal nuclear reaction of this star, which is also the criterion for determining the luminosity of the star.

The relationship between brightness and magnitude is artificially prescribed, because the perception of brightness by the naked eye obeys the logarithmic law rather than the linear law, so it does not mean that if the brightness is increased by 2 times, we will see that it is also so much brighter with the naked eye.

Astronomy stipulates that the brightness of every 5 magnitudes differs by a factor of 100, and it is exponential, that is, it is equivalent to exponential.

This base is constant, and the 5 of the exponent is the magnitude difference, and 100 is the multiple.

So, if a star has a supernova explosion and its brightness increases by a factor of 10 billion, which is to the fifth power of 100, in other words, the star will have a magnitude of 25 and will become a shining star in the night sky, and may even be illuminated by night as day.

Absolute magnitude is the brightness of a star measured by assuming that it is placed 10 parsecs (light-years) from Earth. It is used to distinguish it from apparent magnitude. It reflects the true luminous ability of celestial bodies.

If the absolute magnitude is denoted by m, the apparent magnitude is denoted by m, and the distance of the star is the number of parsecs r, then m=m+5-5lgr.

Calculation examples. Betelgeuse has an apparent magnitude of +, and at a distance of 773 light years, its absolute magnitude is: mBetelgeuse.

5*log10(

Vega's parallax is:", apparent magnitude+, then its absolute magnitude is: M Vega.

log10(

Parallax of South Gate II", absolute magnitude +, then its apparent magnitude is: m south gate two.

log10(

r = distance, m = absolute magnitude.

R1 = according to M = M + 5-5lgr

m1=msun=

m=(m1-msun) power.

If only the apparent magnitude of the Sun is given, the formula m=m+5-5lgr can be used again. Calculate msun

I don't have a scientific calculator at hand, so let's do the math yourself.

Summary. You don't need to do the math, it's just a 10-second difference. Because the annual parallax of a star is 1", then its distance is 1pc (parsec).

If a star's annual parallax is", then its distance is 10pc (parsec). If a star's annual parallax is", then its distance is 100pc (parsec). And so on.

You don't need to do the math, it's just a 10-second difference. Because the parallax of a star's anniversary stocking is 1", then its erection distance is 1pc (parsec). If the parallax of a star is chronological", then its distance is 10pc (parsec).

If a star's annual parallax is", then its distance is 100pc (parsec). And so on.

You don't need to do the math, it's just a 10-second difference. Because the parallax of a star's anniversary stocking is 1", then its erection distance is 1pc (parsec). If the parallax of a star is chronological", then its distance is 10pc (parsec).

If a star's annual parallax is", then its distance is 100pc (parsec). And so on.

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Summary. Hello, dear, the parallax of a sidereal anniversary is, and its parallax is equal to; You don't need to do the math, it's just a 10-second difference. Because the annual parallax of a star is 1", then its distance is 1pc (parsec).

If a star's annual parallax is", then its distance is 10pc (parsec). If a star's annual parallax is", then its distance is 100pc (parsec). And so on.

Hello, dear, the parallax of a sidereal anniversary is, and its parallax is equal to; You don't need to do the math, it's just a 10-second difference. Because the annual parallax of a star is 1", then its distance is 1pc (parsec). If a star's annual parallax is", then its distance is 10pc (parsec).

If a star's annual parallax finch silver letter is", then its distance is 100pc (parsec). And so on.

You don't need to do the math, it's just a 10-second difference. Because the parallax of a star's anniversary stocking is 1", then its erection distance is 1pc (parsec). If the parallax of a star is chronological", then its distance is 10pc (parsec).

If a star's annual parallax is", then its distance is 100pc (parsec). And so on.

The annual parallax of a star is, its parallax is equal, and the absolute magnitude is how many parsecs apart from it is.

4.Please use the deflection of latitude and longitude lines to explain the deflection of horizontally moving objects on the earth (without drawing).

Both are shifted to the west, which is due to the influence of geostrophic deflection forces. You have to understand that the geostrophic deflection force is due to the rotation of the earth, and the objects moving on the surface of the earth are shifted to the right in the northern hemisphere and to the left in the southern hemisphere. Then the movement from the high latitudes of the Northern Hemisphere to the low latitudes of the Rang Core is the movement from north to south, and the direction on the map is the downward movement.

When you go to the right, you go west. The high-latitude to low-latitude movement of the Southern Hemisphere is from south to north, which is shown on the map as an upward buried movement, with the tan-liquid excavation deflecting to the left and the same deflection to the west.

Summary. Hello, for your question [Knowing that the brightness of the sun reaches -, calculate how many times the brightness of the sun is the brightness of a first-magnitude star] The answer to this question is as follows: First, the difference between each magnitude is multiplier, and the sun is a 27th magnitude star.

Just use 27-one equals 26. Use it all over.

Hello, for your question [Knowing that the brightness of the Sun is up to -, calculate how many times the brightness of the Sun is the brightness of a magnitude star] This question gives you the following answer: First of all, the difference between each magnitude is multiplier, and the Sun is a star of 27th magnitude. It was made at 26 with a 27-first class beat.

Everywhere you go. According to the measurements, the magnitude of the sun reached an astonishing staggering sensation! If you do the math, you can see that it is a trillion times brighter than the faintest 6th magnitude star.

Using the conversion formula: m = m + in seconds, 1 second = light years, and absolute magnitude is the apparent magnitude of the star when it is 10 parsecs away from the observer. 1 astronomical unit and other states are light-year, replaced by a second difference, equal to the second difference, substituted into the formula, and the abacus is out of order.

First of all, the difference between each magnitude is multiplier, and the Sun is a 27th magnitude star. Just use 27-one equals 26. Use it all over. It's the result, it's like this.

There is a formula, absolute magnitude is denoted by m, apparent magnitude is denoted by m, and the distance of the star is reduced to the number of parsecs r, then m=m+5-5log(r).

Apparent and absolute magnitudes can be converted using the formula, which is as follows:

m＝m＋5－5 lg d

m is the absolute magnitude; m is the apparent magnitude; d is the distance.

We call the visual brightness (i.e., apparent magnitude) seen from a distance of 10 parsecs from the star the absolute magnitude of the star. The Sun is of absolute magnitude.

Calculated according to the formula.

lg 100

m = i.e., the magnitude of the star is equal.

Using the conversion formula: m = m + in seconds, 1 second = light-years, and absolute magnitude is the apparent magnitude of the star when it is 10 parsecs away from the observer. 1 astronomical unit is equal to light years, replaced by a second difference, equal to a parsec, substituted into the formula, calculated.