What is the art of studying stars?
147023
astronomy (uranology)\nastrology
333315
Close your eyes then wish upon a star !! That should do miracles for you !!!
354510
By stars, you mean women, and by telescope, you mean co-ck right?\n\nAnd yes.
1088976
here you go:\n\nhttp://www.enchantedlearning.com/subjects/astronomy/stars/startypes.shtml\n\nFrom your list it would be nova, but that is for a (relatively) short period of time.
496226
STARS AND NEBULAE.\n\nMost of the things you can see in the night sky are stars: a few thousand are visible to the unaided eye. A star is a hot ball of mostly hydrogen gas; the Sun is an example of a typical, ordinary star. Gravity keeps the gas from evaporating into space, and pressure due to the star's high temperature and density keeps the ball from shrinking. In the core of the star, the temperature and densities are high enough to sustain nuclear fusion reactions, and the energy produced by these reactions works its way to the surface and radiates into space as heat and light. When the fuel for the fusion reactions is depleted, the structure of the star changes. The process of building up heavier elements from lighter ones by nuclear reactions, and adjusting the internal structure to balance gravity and pressure, is called stellar evolution. \nLooking at a star through a telescope can tell us many of its important properties. The color of a star tells us its temperature, and the temperature depends on some combination of the star's mass and evolutionary phase. Usually, observations also allow us to find the luminosity of the star, or the rate at which it radiates energy as heat and light. \nAll stars visible to the unaided eye are in our galaxy, the Milky Way. The Milky Way is system of roughly 100 billion stars, along with a great deal of interstellar material. The galaxy is shaped like a flattened disk embedded in a round, faint halo. Gravity keeps the stars from drifting away, and the motions of the stars keep the system from falling in on itself. The Milky Way has no distinct edge - the distribution of stars tapers off gradually with increasing distance from the center. The SDSS detects stars more than a million times fainter than can be seen with the unaided eye, far enough to see the outer structure of the Milky Way. \nStar Colors and Luminosities: The H-R Diagram\nAstronomers often make plots of the luminosities of stars compared to their colors. The first such charts were made in the early twentieth century, when astronomers took spectra of thousands of stars, then placed the spectra into a sequence based on the appearance of several different features. The classes of stars were given different letters as names; in order of decreasing temperature, they are OBAFGKMLT. The hottest stars are class O, while the coolest are class T. Two astronomers, Ejnar Hertzsprung and Henry Norris Russell, independently started to wonder what would happen if they compared stars' luminosities to their spectral classifications (or, alternatively, to their temperatures). They knew that some stars were hotter and more luminous than the sun, and that others were cooler and less luminous. Hertzsprung and Russell found that 90% of the stars fell into a narrow band they termed the "main sequence." Today, we call this type of plot a Hertzsprung-Russell (or H-R) diagram. \nAstronomers further divide each letter into ten categories from 0 to 9, with 0 being the hottest star in that spectral class and 9 being the coolest. So, a B1 star is hotter than a B2 star, and a B9 star is hotter than an A0 star. Our own sun is at the "hot" end of the G range with a surface temperature of 5,770° K; therefore, it's called a G2 star. \nSpectral classes give us a convenient way to refer to most types of stars - from O0, the hottest at over 25,000° K, down to T9, the coolest failed stars at 1,000° K. Each spectral type of star is associated with a specific color: all G-type stars like the sun are yellow, all M-type stars appear red, and all B-type stars are bluish. Thus, this system of letters and numbers tells us where a star is on the horizontal (color or temperature) axis of the H-R diagram. \nTwo alternative systems tell us approximately where on the vertical (luminosity) axis a star can be found. One system uses absolute magnitude, a measure of luminosity derived from the apparent magnitude, or brightness of the star
200341
To start with the chioces are good enough.\n\nHowever, for their use keep in mind that you won't be able to see stars. What you can see is reach to the moon, planets, settellites of different planets, steroids and and man made settelites. \n\nFor these observations you will need assistance of different maps and schedule of movements. This will enable you to go to higher observations. \n\nYes the first advice is good, join a club, read books and be in contact at internet.
604233
By using spectra. Each element has characteristic frequencies of light that it emits or absorbs. If light from the star is spread out into a spectrum (like a rainbow), there will be dark lines for absorbtion and bright lines for emission. By identifying the chemicals that correspond to those lines, we deduce the composition of the star.
260019
Everything about space is interesting. It is all a mystery and so much is yet to be discovered. I used to love to study the planets when I was in school. I love to watch the stars and wonder what is up there and what it is really like to be billions and billions of miles away from the earth
201708
Several different ways depending on the distances involved.\n\nFor close stars, we look at where the star appears to be in the sky at times about half a year apart. Think of looking at your outstretched thumb through your left eye, and then your right eye. The thumb appears to be in a different position with respect to a distant building. In the same way, a star will appear to be in a slightly different position when we look at it from different ends of the earth's orbit. The amount of shift depends on the distance to the star and that allows us to figure out the distance. This method is called paralax.\n\nFor slightly more distant stars, we look at clusters of stars and measure their apparent motion across the sky over a course of *years*. Just as train tracks appear to converge at the horizon, the motions of the star will appear to converge. The rate of convergence is related to how far away the cluster is.\n\nWith these methods, we get enough stars to do statistical analyses of the brightness of the stars versus their chemical composition and other aspects of their spectrum. With this knowledge, we can estimate the distances to further stars by just comparing their spectrum to that of already measured stars. Scientific models of stars are used at this stage.\n\nFarther away than this, we look for 'standard candles', that is, stars of known brightness. By comparing the brightness they appear to be versus their actual brightness, we can estimate their distances. A particular type of 'standard candles' are the Cepheid variables. Their actual brightness depends on how fast they vibrate. Since we can see these stars in other galaxies, we can use them to determine the distances to those galaxies.\n\nFinally, after we know the ditances to some galaxies, we can measure the rate at which they move apart as a function of distance. By measure red-shift (hence speed) of more distant galaxies, we can determine their distances.
768736
180°\n\nYesterday it was asked about a 5-pointed star.\n\nWell let us look at an n-pointed star\n\n1. Draw the circumscribing circle\n\n2. Join the vertices and create a regular n sides polygon inside the circumscribing circle\n\n3. Join each vertex to the centre\n\n4. Each point of the star is half the ange at the centree subtended on the same side.\n\n5. Each angle in the centre is equal as they are all subtended by equal chords as the sides of a regular polygon are equal.\n\n6. The sum of the angles at the centre of the circle = 360°\n\n7 So the sum of the angles at the circumference \n= sum of the angles of the star \n= ½ of 360°\n= 180°\n\nBONUS\n8 So each angle = 180°/n\n\nIf n = 5 each angle = 36°\nIf n = 7 each angle = (25 5/7)°
331089
Let’s start with a couple basics…\n\nWe see basically the same stars (throughout the course of a year, if not night to night) as our ancestors saw thousands of years ago.  Furthermore, all the stars we see in our night sky are part of the Milky Way Galaxy; the most distant stars we can spot without the aid of a telescope lie perhaps a few thousand light years away and most lie within a few hundred light years.  That means that the light from these stars took only a few hundred (or at most a few thousand) years to reach us.\n\nStars live for millions or billions of years, so although the light we’re seeing on a starry night is perhaps tens or hundreds (or maybe thousands) of years old, that’s not much compared to the lifetime of a star.  So the stars we see haven’t changed much in the time that it’s taken for their light to reach our eyes on Earth.  In the millennia that people have observed the sky, maybe one or two or a few stars have flashed “on,” and a similar number may have flashed “off,” but you’d be hard pressed to find even a single example in all of recorded history.\n\nStars indeed move over long periods of time (we’re talking about changing the shape of constellations here, not just seeing stars rise in the east and set in the west as they do every night), so over hundreds of thousands of years, one could see the Big Dipper distort into a different shape.  But again, this happens on a time scale much longer than a human lifetime—and again, longer than recorded history. \n\nSo the stars (and the patterns we see them form, the constellations) stay pretty much the same—not only as long as we live, but as long as our cultures have existed.  So the “Three Kings,” by which I’m guessing you mean the three stars in the belt of Orion, will be easy to spot for as long as you decide to go out star-gazing.\n\n\nRyan Wyatt\nRose Center for Earth & Space\nNew York, New York
809888
All stars are round, and there are many trillions of stars, although you can only see about 3,000 of them at any one time without a telescope. The sun is a typical star, only much closer than all the others.
1145113
This should help you:  http://www.le.ac.uk/physics/faulkes/web/stars/o_st_overview.html
1095458
You can't actually "buy" a star, but you can name one. There are plenty to go around ya know.\n\nCheck out these websites:\n\nhttp://www.starregistry.com/\nhttp://www.nameastar.com/
666465
There are a couple of ways. One uses diffraction effects or speckle interferometry to estimate the angular size of the star. Once the distance to the star is known, the actual size can be determined fairly easily. This method can only be used for very large stars (such as red giants) or very near stars.\n\nFor other stars, we determine the temperature of the star via the spectrum. This tells how bright the star is per unit area. Then, we look at the distance and apparent brightness to determine how bright it is overall. Dividing will give the surface area of the star, and hence its size. The difficult here is that the temperature of the 'atomosphere' is usually much higher than the surface of the star and this can significantly affect the estimates. Also, if the star isn't spherical (because of rotation, for example), the surface area alone won't give all the information about its size that might be desired.
645879
Sirius (the Dog Star)\n\nList of the 100 Brightest stars:\nhttp://en.wikipedia.org/wiki/List_of_brightest_stars
564481
astrology is the study of the stars and planets and horoscopes is predicting someones fate by using the position of the planets and stars at a certain time.