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COURSE Introduction to Astronomy (46)

double and multiple stars.

Many stars like Aldebaran, Antares, Rigel, Polaris, etc at first glance appear as a single point of light, observed telecospio are formed by two or more stars next to each other. These stars are called double if two triples if they are three, and if more, they are called, in general, multiple.
double stars are divided into:
1) optical Doubles: When are composed of two stars located far distiancia independently of one another and who are next projected on the celestial sphere by the effect of perspective.
2) physical or binary Doubles: When between the two stars there is physical linkage, that is, they spin around each other under the laws of Kepler and Newton, forming a binary system.
In some double stars, the components are so close that even with the most powerful telescopes they appear as single stars and are known to be double by spectral analysis, or by the darker eclipses of the components produced wholly or partly the brighter the star appear as a variable, such as the star Agol. Among the stars
triples have to Regulus, including Lyra multiple.

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COURSE Introduction to Astronomy (45)

Variable stars

A large number of stars will not shine steadily, but will vary periodically, or whatever it is, do not retain the same apparent magnitude and in a shorter or longer period and more or less regular, their magnitudes reach different values, such stars are called variables.
For example, the star Mira Ceti (constellation of the whale), which historically was the first known variable star in a period of 332 days passed from 2 nd to 9 th magnitude.
With the use of photography in astronomy, he discovered so much better the variability of the stars, so it was photographed the same region of sky in two different dates with the same instrument and in identical positions, comparing the two pictures can be seen if the stellar image varies or not.
Variable stars are classified as:
1) Intrinsic: those in which their magnitude variations due to changes in the star's internal structure, and that changes color, temperature and range, along with these changes of light .
2) Extrinsic: not regarded as real variables, since variability of sun light is produced by external physical causes unrelated to the star itself. According
cuva variability of the stars, they are divided into:
1) Periodic or regular: the light curve is periodic, ie, after an interval of time, called period, plays unalterably.
2) semiregular: ligeramnete period is variable and the curve is reproduced with low accuracy in each period.
3) Irregular: in these there is only one small indication of periodicity.
Observing variable stars is one of the most interesting work programs for the amateur astronomer. NO requeire costososy use of instruments made, and often most suitable for visual observation using binoculars or a 60 mm refractor. The work of variability is to define the range of variation of brightness and the period of the variable in question. For those observers who want to delve into this area to get in touch with major international organizations variable stars, and that through their newsletters, online via email or we can read the latest news that most interest us. These organizations also distribute some star charts to find the variable to consider, among other important features

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STELLAR MAGNITUDE (2)

The absolute magnitude of a star is the magnitude I would have said star if it were located at a distance of 10 parsec (1 parsec is 3.2616 years = 3.0857 X10 light 16 m, ie the distance from which Earth and the Sun would seem to be separated by an angle of 1 arc second) .
The magnitude of the stars is now known through the photometers or photographically.
is the term applied to the first magnitude stars that range from + 0.6 to 1.5, the second magnitude of the stars of + 1.6 to + 2.5; third magnitude from + 2.6 to + 3.5, etc.
The number of stars visible to the naked eye is about 6,500, with 20 stars of 1 magnitude, about 60 of 2 nd magnitude star close to 200 3 rd magnitude approximately 600 4 th magnitude, about 1,600 stars 5 º size and more than 4000 of 6 th magnitude. Assuming that the stars are distributed equally in the sky, an observer in an instant see about 3,000 stars.

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COURSE Introduction to Astronomy (43)

STELLAR MAGNITUDE. (1)

The record of the positions of stars in a catalog called esteleares lists is a fundamental baseline for important astronomical knowledge such as the determination of the time, the phenomena of precession and nutation, proper motion of stars. The earliest catalog was developed by astronomer Greek Hipparchus in 127 BC It contained the positions of 1080 stars divided into six classes according to their apparent brightness Arabs kept another catalog of stars called "Almagest" of Ptolemy, in this work we have inherited the custom to group the stars brightness classes or magnitudes. The classes of brightness were called magnitude, calling for the brightest of 1 st magnitude, 2 nd, 3 rd, 4 th, etc., until the 6 th magnitude, the latter are the faintest stars that distinguish somple view.
For magnitude means the apparent brightness of stars we see and dimensions of these stars.
In 1856 the astronomer Norman Pogson established the "Pogson scale" means a 1st magnitude star has an apparent brightness 2,512 times greater than a 2 nd magnitude star, this 2,512 light intensity greater than a 3 rd magnitude and so on. Pogson included the star Aldebaran and Altair to the base times the scale. These magnitude scales extending one hand toward zero and negative numbers, to encompass the brightest stars like the Sun and the Moon.
The apparent magnitude depends on the brightness of the star and the distance that is an example, Sirius has an apparent magnitude of -1.46 (the most brilliant of heaven, is to 9 light years away, while that Rigel is 2000 times more luminous, with a magnitude appears to be 0.08 at a distance 100 times greater).

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NAME AND TITLE OF THE STARS.

From the earliest civilizations, the stars are considered grouped into constellations. The names of the stars both from the Greeks such as Sirius, Procyon, Pollux, Castor, Regulus, Polaris, Arcturus, Canopus, The Pleiades, as the Arabs and the names of Alcor (weak), Mizar (veil) Vega (fall), Aldebaran (the follower), Deneb (the tail), Rigel (leg) Algol (star demon), Betelgeuse (shoulder Giant), and a few hundred names.
Unable to give nEombre to the huge number of stars raised the idea of \u200b\u200banother system of nomenclature that is most useful to astronomers.
In 1603, Johannes Bayer of Germany published a book called Uranometría, an atlas of star maps which showed the stars in each constellation alafabeto using Greek letters that followed the genitive of the Latin name for the constellation to which it belongs. Bayer
established an order of brightness within each constellation, so called to the brightest star, b which was brighter, g to the next and AASI on. The drawback of this classification is that only the Greek alphabet has 24 letters, while on average there are about 70 visible stars for each constellation. When the Greek alphabet were insufficient for a constellation Bayer resorted to the use of the lowercase letters of the Latin alphabet, complicating the method.
After the appearance of the telescope showed the existence of a greater number of stars and was raised again the issue of its name.
In 1712, the English astronomer John Flamsteed, was the first catalog with the help of the telescope, called Coelestis History Britannica, resorted to the use of numbers instead of letters, numbers assigned to each star according to the order in which they reached the meridian. Eventually
were improved telescopes, observing and millions of stars in each constellation, the stars are distinguished not by name, or letters, or numbers, if not by their position on the celestial sphere, ie by right ascension and declination.

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meteors.

A meteoroid is a piece of material, of variable size and shape located in interplanetary space may be attracted by the gravitational field of the earth and land on our planet.
Friction with the atmosphere there is a sharp rise in temperature causes a luminous phenomenon, visible, known as a meteor or shooting star.
When a meteor reaches a high brightness (magnitude -4 or higher) is called bólido.Por Finally, when a meteoroid manages to reach the earth's surface is called a meteorite.
For meteors visible with a magnitude of between 1 and 6 have a weight between 2 mg and 2 grams. But there are many smaller fragments that cause meteors undetectable to the naked eye, being the total amount of matter falling into a meteoric day on Earth, between 1000 and 10000 tons.
sporadic meteors can appear anywhere in the sky, or forming the so-called meteor showers. Any clear night is suitable for the observation of sporadic meteors, but are more frequent in the second half of the night.
During a meteor shower, meteor rate is usually higher. Some have come to rely 2,000 meteors per hour. If during a meteor shower meteor traces are represented in a star map, we see that they all seem to come from a point, that point is called radiant. Meteor showers are named for the constellation which is the radiant is located, such as Leonidas, whose radiant is located in Leo, Taurid (in Taurus), the Orion (in Orion), Persians (in Perseus), etc ...
As for the origin of meteor showers, they are associated with the cometary orbits, occur when the Earth crosses the orbit of a comet. The swarms of meteoroids and debris are remnants of comets that orbit the Sun in elliptical orbits. Sporadic meteors are caused by meteoroid swarms of old waste.

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asteroids.

In 1920, K. Hirayama noted that some asteroids had some of their orbital elements grouped in the family. A family comprising a main asteroid which gives its name and a tag associated with much smaller asteroids. For example, the family associated to 8 Flora (160 km) is the most popular and populated as it is known more than 400 members, the family of 24 Themis (200 km) has 150 members, of which three are over 100 km . as 90 Antiope, 268 Adorea, 171 Ophelia.
At the orbit of Jupiter, about Langraje points, one at 60 ° before the gas giant and the other at 60 degrees behind it, is a group of asteroids called Greeks and Trojans each other.
If a diagram is represented in abundance asteroid as a function of distance from the Sun, is that the distribution is discontinuous, gaps or voids exist asteroid, caused by the gravitational action of Jupiter. These gaps or sparsely populated regions of called "Kirtwood Lagoons." The classic explanation is that the attraction of Jupiter eliminates the effect of resonance orbits whose period is a rational fraction of theirs. For example, objects that have a semi-major axis of 2.50 AU, run three laps around the sun at the same time that Jupiter runs a twist: the resonance 3 / 1, other resonances are 2 / 1, 3 / 2. The farther away from the main belt stabilizer is more resonance.
Today know one small asteroids whose orbits are very close to Earth's orbit at high speed, are called "Aten-Apollo-Amor" and distinguished into several categories:
1) The bodies whose orbits pass close to the planet Mars and the asteroid Hungaria.
2) objects whose perihelion is closer to the Sun than Mars, often called "Mars-crossers." These are subdivided into four subsets:
2.1) Those who do not come to less than 1.20 AU from the Sun
2.2) Those that pass near the Earth but not deep into Earth's orbit, its prototype is 2.3
Love 1221 ) Those who enter the Earth's orbit and have a longer period a year. Its prototype is 1862 Apollo.
2.4) Same as 2.3 but with an orbital period less than one year. Typical example: 2062 Aten.
must know that 75% of the asteroids are concentrated in the zodiac (defined as a band of apparent width 15 ° centered on the ecliptic). Most of them are too weak to be detected by an amateur telescope, only a few, the brightest, m can be realized. For this, consult the ephemeris of astronomical journals and astronomy software.

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asteroids.

The conjunbto asterioides constitute a large and heterogeneous, small stars, also called minor planets, irregularly shaped, which orbits around the Sun, most of whom are between the orbits of Mars and Jupiter in the so-called main belt. An asteroid is a small rocky body orbiting the Sun with a diameter of less than 1000 km.
The first asteroids were discovered by chance, when engaged in finding the missing planet by looking between the orbits of Mars and Jupiter. Only 10% of them have a considerable size, such as the greatest of all and the first to be discovered on January 1, 1801 in Palermo (Italy) is Ceres, which has a diameter of 1,020 km, and Vestas Pallas cpn an approximate diameter de540 km in 1845 discovered five asteroids. Ten years later, and forty asteroids were discovered. With the application of photographic techniques, around 1845, it was discovered 15 asteroids per year, twenty asteroids per year in 1910, forty per year in 1930 ...
The relative velocity reaching these asteroids in the main belt is 5 km / sec. The collisions, when they occur, violent and destructive. Asteroids are thought to have endured more robust than several successive cycles of destruction-reconstruction.

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TAILS OF COMETS

a comet's tail also causes the Sun's first astronomer who realized the importance of the Sun in the development of this phenomenon was Peter Appian, who found that comet tails are always deployed in the direction opposite the sun
often observed in the same comet two different queues: a tail of dust and other so-called ion tail. Dust tails are curved lines, are formed by dust particles torn from the coma by solar radiation pressure and away from the coma. The ionic lines are rectilinear lines (or very weak curvature) caused by social radiation that ionizes the molecules of the coma aquires electric charge, magnetic fields and solar wind drag away from the coma these molecules forming the ion tail.

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THE CLASSIFICATION OF COMETS.

The comets are designated by a nomenclature, ie the name of its discoverer / s (maximum three discoverers), followed by the year of discovery and a lowercase letter indicating the number of order appearance of the comet within the year. When one considers the orbital data of the same, the year is replaced per year of perihelion passage, followed by a roman numeral indicating the order number that step.

For a comet should be visible close to the sun, this causes changes in the kite making it visible to the telescope, if weak, or if it's bright eye. Typical and morphologically

a comet consists of:

1) Nucleo.
2) Eat or hair.
3) tail or tails.

often appear devoid of comet tails, particularly those who have already taken many turns to the sun gradually losing some of its mass. In other cases show a spike or spike on the opposite side to the tail. The most widely accepted among astronomers is that the core is a dirty snowball, assuming that the nucleus of a comet is a ball of ice mixed with dust particles. The dimensions of the core can vary between 1 and 100 km.
When a comet approaches the Sun, solar radiation, evaporation of the ice cream core material. In this evaporation process arising paricular thus forming a dust cloud of gas and dust surrounding the nucleus. This cloud is the comet's coma coma diameter can reach 100,000 km.
The coma is visible through two processes: first, the comet's dust reflects sunlight, on the other hand, the molecules dissociate gas due to solar radiation and become fluorecientes, emitting light.

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THE ORBIT OF COMETS.

Comets can describe three types of orbits:

1) ellipticals.
comets whose orbits are elliptical with periodic character, moving around the Sun, which occupies one focus. As a rule, their eccentricities are large. Some comets have relatively short orbital periods as in the case of comet Encke, with a period of 3.3 years while others have hundreds of years.
Because comets have masses very small gravitational influences of the planets with almost nil. On the contrary, due to the gravitational perturbations of the Sun and some giant planets, Jupiter and Saturn in particular is very common that the comet's orbital period alters, through changes, sometimes dramatic. One of the disturbance is the capture of comets by planets, which can be placed aphelion far beyond Pluto (periodic comets) by transforming them into short-period comets than they did, whose aphelion is within the Solar System. Catch these families originate from comets like Jupiter, made up of more than 60 members whose aphelion is located near the orbit of Jupiter. There are also families of Saturn, Uranus, Neptune and Pluto.

2) Hyperbolic.

3) Parabolic.

Comets with parabolic and hyperbolic orbits are not periodic since their curves are not cerradas.Luego appear only once emerging from the depths of space, they approach the sun and away from it and disappeared forever.
The orbit of comets have very different angles on the plane of the ecliptic. Guna them to have an inclination greater than 90 ° so that the comets that have moved in a retrograde, such as Halley's comet.

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comets. Formerly

to comets have been related to adverse events, wars, epidemics. The word comet comes from the Greek for "hair", referring to the morphology of these stars.
Currently, the most accepted hypothesis is that made by the astronomer Oort, that there is a vast region of space located between 40,000 and 150,000 AU in which there are 100,000,000,000 cometary nuclei, called the Oort Cloud. Due to sporadic disturbances caused by the next step of some star, some of these nuclei can be propelled into the Solar System. One of them would approach the Sun as hyperbolic or parabolic orbits and move away then disappearing. Other cores, due to the gravitational influence of the Sun and planets like Jupiter and Saturn, would be captured and become periodic elliptical orbits. After completing a large number of orbits and revolutions around the Sun and would have spent their stuff and would eventually disappear by the continuous wear.

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MUTUAL PHENOMENA of the Galilean satellites

Jupiter, the largest planet in our solar system, currently has 17 satellites. The first four: Io (a satellite with volcanic activity), Europa, Ganymede and Callisto were descubietos by Galileo Galilei. In her honor these four moons are called the Galilean satellites.
The four Galilean satellites can be observed with optical medium, and assessed the following events or details:
1) ECLIPSES: produced when a satellite enters the shadow of Jupiter.
2) Hide: those that are produced by a satellite passing behind the planet Jupiter.
3) STEPS: occur when a satellite is interposed between Jupiter and Earth.
4) STEPS OF SHADOW: are caused by the projection of the shadow of a satellite on the planet.

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apparent position of the outer planets.

outer planets are those located further away from the Sun than the Earth. They are: Mars, Jupiter, Saturn, Neptune, Uranus and Pluto.
When the Earth and outer planet are on opposite sides of the Sun, says that the planet is in conjunction. This is the time when the planet is behind the sun, making it impossible to observe. It is said that an outer planet is in opposition when the planet is at its closest position to Earth, this is visible all night: The Sun sets in the west and the planet rises in the east. As time passes, the planet rises until it sets in the west, more or less at the time the sun will rise in the east.
You can see a planet during the time that is not in opposition. The closer you get less time to their conjunction can be seen in the sky. It is said that an outer planet is in quadrature with the Sun when the angle of the planet Earth and the Sun at a right angle of 90 degrees. You can observe a phase effect on some outer planets.

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COURSE Introduction to Astronomy (32) COURSE A LA

Danjon SCALE

During the eclipse the Moon has a degree of visibility known as the Danjon Scale.
0 = Very dark eclipse, the Moon is almost invisible.
1 = Eclipse, gray or brown. Eclipse
2 = dark red or rusty color, shadow edges clear. Eclipse
3 = brick red, or yellow light shade. Eclipse
4 = very clear, coppery red with blue trim.

eclipsed Moon can stay for 1 hour, 45 minutes maximum, then the Moon out of the shade with a small growing light, will widen to the left of limbo, until the shadow leaves the disk and then the darkness is lifted. The eclipse is over and can last about six hours.

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MECHANISM OF AN ECLIPSE OF MOON

Lunar eclipses are caused by interposition of the Earth between the Sun and the Moon, ie, when the Earth's shadow falls on the Moon, and occurs necessarily on a full moon. The Sun and Moon in opposition, ie, diametrically opposite in the sky with respect to the Earth as a lunar eclipse requires alignment the Sun, Earth, Moon.
If a spherical opaque body is placed before a light source also spherical, the boundary of the shadow will be the conical surface tangent to the two bodies and appear shaded areas and shadow areas. The shadow ring is substantially the same width as the Moon and the diameter of the shadow is nearly triple.
In the case of a lunar eclipse, the Sun is the light source and the Earth is opaque body. For the Moon enters the shadow cone is necessary that the Moon is in opposition and at Full Moon or Full Moon. If the whole moon enters the umbra will be a total lunar eclipse, if not enter a part, will be a partial lunar eclipse.
If the lunar orbit plane coincide with the ecliptic, in each competition or full moon, there would be a lunar eclipse. But remember that the plane of the lunar orbit is inclined 5 º 8'respecto of the Ecliptic and therefore the umbra will sometimes below and other above the moon, then there will be no eclipse of the moon. When there is an opposition and Moon encientre the node (when the moon's latitude is zero) or close to it, then there will be a lunar eclipse.
The lunar eclipse you can see all the observers who see this item on the skyline. Copper dyes are observed in a total lunar eclipse is due to the refraction of sunlight in Earth's atmosphere, casting shades on the Moon comparable to those of a setting sun lighting the moon during an eclipse depends on our atmosphere: dust, volcanic ash suspended in eclipse darkens the air.
The edge of the Moon is dark, with no significant first so then it is more noticeable. After an hour the Moon has entered fully into the penumbra of the Earth and has lost luster. See a black notch biting the edge of this, is the entry into Earth's shadow. Notch increased progressively and in an hour and has engulfed the entire lunar disk.
At first, the shadow is blue-gray and as surrounding the lunar disk becomes red. A total eclipse from dominating the red, but the tone varies in the course of the phenomenon.

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EXPLANATION OF PHASES LA LUNA

Over time the zone light will enchancha and spend a week since the New Moon, the Moon is 90 degrees from the sun (the moon is square) and is in Phase Waxing Crescent seeing crescent-shaped illuminated . His age is 7 days, 9 hours, 11 minutes and 0.72 seconds in this position, the moon passes the meridian of the place about 6 hours of sun
In successive days, the straight edge by increasing the illuminated curve until two weeks after New Moon or Full Moon Full Moon seeing the whole disk illuminated. His age is 14 days, 18 hours, 22 minutes and 1.45 seconds. The Moon passes the meridian at midnight and is in opposition (the Earth is situated between the Sun and the Moon). The lengths of the Sun and the Moon differ 180 degrees. The observer, located on the dark side of Earth is the night for him, you see the whole face of the moon illuminated. At Full Moon, the Moon is said to decrease.
spend a week at Full Moon, the Moon is Last Quarter, and it looks like a semicircle but the diameter to the east (right). The age of the Moon is 22 days, 3 hours, 33 minutes and 2.2 seconds. Is when the moon is 270 º of the Sun (the Moon is square again.)
Over time, the Moon will be in the form of a piece but with the horns to the right, until finally at the age of 29 days, 12 hours, 44 minutes and 2.9 seconds, limited to one synodic month, we get to the new moon that marks the beginning of another lunation.

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moon phases.

moon phases are called to the various aspects under which the Moon appears to depend on the relative position of the Sun, Earth and Moon, in a cyclical proceo determined by the various states of enlightenment in which shows the lunar disk. If you watch me to the moon on successive days we see their apparent shape varies from day to day.
The period of this cycle or lunation is a synodic month. To explain this phenomenon assume phase to earth at the center of a circle that represents the lunar orbit. Assuming the Sun on the right, the hemisphere of the Moon that appears to be illuminated and dark sun reversed.
The origin of the lunar cycle is in the so-called new moon or new moon, when the moon is in conjunction with the Sun at this time starts a synodic revolution. The Earth Moon presents the hemisphere not illuminated by the Sun, and is dark, therefore, we see the moon. Age is called the Moon for a given time of the lunation the time between the New Moon (age = 0) and that instant. The rising and setting of the moon and the sun almost coincide, as well as the passage of these stars over the meridian. Having the moon a proper motion journal close to 13 º in the forward direction, while the Sun moves 1 to day, the Moon moves with respect to the sun about 13 ° per day and, therefore, 2 or 3 days after new moon is submitted after the setting of the sun in the form of thin spindle, and a piece with horns to the left.

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Libration of the Moon.

As the orbit is ecliptic and the axis of rotation is inclined from the perpendicular to the orbital plane, there is an effect known as libration (in longitude and latitude) that we can see from our planet a little more than half of the lunar surface (59%).
The libration in longitude because the Moon rotates uniformly about its axis, while the orbital motion is faster near the perigee Maas and slower near the peak (by Kepler's second law). Therefore, a lunar surface detail, which at perigee and apogee is located right on the meridian of the place, find something to the east of the meridian when the Moon is between the perigee and apogee, and slightly to the west when it is between the apogee and perigee.
This implies that we see over 50% of the area lunar.El period of libration in longitude is equal to the anomalistic month.
The libration in latitude is due to the inclination of the lunar rotation axis perpendicular with respect to the orbital plane. The period of libration in latitude is equal draconítico month.
The night or parallactic libration depends on the place of observation on the surface of the Earth: two observers who are in two different points on the earth's surface at one time see something different regions of the lunar surface.

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revolutions of the moon.

The period of movement of the Moon around the Earth can be seen in different ways: 1 .-
sidereal month: it is the time between two consecutive steps of the Moon by the hour circle of a star seen from Earth. Its duration is 27 days, 7 hours, 43 minutes and 11.6 seconds. It matters little astronomy and its value is calculated as the semi-major axis of the orbit. 2 .- synodic
Month: The time elapsed between two similar positions of the Moon and the Sun, ie between two phases of the moon. Its duration is 29 days, 12 hours, 44 minutes and 2.9 seconds and deconomia lunation. 3 .- Month
tropics is the time between two consecutive steps of the Moon by the hour circle of Aries point. Its duration is 27 days, 7 hours, 43 minutes, 4.7 seconds. 4 .- anomalistic
Month: is the time between two consecutive steps of the Moon perigee. Its duration is 27 days, 13 hours, 18 minutes, 33.2 seconds. 5 .- draconítico
Month: is the time between two consecutive steps of the Moon by the ascending node of its orbit. Its duration is 27 days, 5 hours, 5 minutes, 35.8 seconds.
The moon has a rotation in the forward direction around its axis, and time spent in a rotation is the same as its sidereal revolution. The rotation length is equal to what it takes to travel its orbit around the Earth, so the Moon always presents the same face to Earth except for slight variations due to librations.

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.- LA LUNA LUNAR ORBIT.

For observers, before embarking on an observation of the Moon, should know its orbit around the Earth, to understand its apparent movement and the various issues that may occur in the sky to an observer on Earth.
The Moon is the astronomical object closest to the Earth. The moon rotates
long around the Earth describing an ellipse in one of whose foci is the Earth with a large tilt igual a 0,05490. Siguiendo este valor, el perigeo (distancia mínima de la Luna a la Tierra) está en 363.296 Km. y el apogeo está en 405.50, siendo la distancia media 384.400 Km. Su semieje mayor es de 384.399,1 Km, la inclinación respecto de la eclíptica es 5,14540 (fracción de grado) o 5º 08´ 43 ,33017´´ (grados sexagesimales). La longitud del nodo ascendente y la latitud del perigeo varían cíclicamente con el tiempo entre 0º y 360º, y no se les puede definir con un valor medio.
La intersección de la órbita lunar y la eclíptica determinan una recta que corta en dos puntos, denominados nodo ascendente y nodo descendente. Sólo en los puntos del nodo ascendente and down results in the phenomenon of eclipses, both lunar and solar. The line connecting two nodes is called line of nodes. This line does not conseva a fixed direction with respect to distant stars, but retrograde in reverse on the plane of the ecliptic the moon's orbital motion with a period of 18.6 years (6793.5 days). As a result, to return to the same node, you must perform at least one complete revolution (month draconícito).
The line joining the perigee and apogee is called the apsidal line. This line has a direct movement and takes place in the lunar orbit plane. Its period is 8.85 years (3232.6 days).

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A TOTAL ECLIPSE OF SUN

continue with the process followed by an eclipse.
suddenly appears the solar corona, appear in the sky the planets and brightest stars. The total is short and the third contact occurs in a similar manner but in reverse order.
Another type of solar eclipse is a hybrid, mixed or worn. Occurs when the tip of the umbra falls short on the surface of the Earth and the event is void, but is changing its project total to finish abort.
Mercury and Venus are the planets closest to the Sun than the Earth, are called inner planets. Proóximo
The planet Mercury and the Sun is moving in the sky faster than any other planet and its rotation period is 58.65 days, ie 2 / 3 of its period of movement around the sun is Venus
the star, following the sun and moon, the brighter the sky, reaching favorable conditions (39 days before or after inferior conjunction) the magnitude -4.4. Because that appears before sunrise or after sunset, is known as "morning star" or "star of the evening."
The maximum angular separation of Mercury is 28 ° and Venus is 47 degrees, therefore never be seen at the zenith of the sky at midnight.
Mercury always appears near the sun, you can watch 2 hours and 15 minutes, at most, before sunrise and after sunset solar. Making it difficult telescopic observation of this planet, since sunlight and prevents or hinders. Venus
also observed before sunrise or after puesta.Al be further from the Sun, is visible up to 4 hours before sunrise and after sunset solar.
Both planets show phases like the Moon. The inner planets have a different geometry of planetary positions to the outer planets. To explain these relative movements consider the sun in the center of two concentric circles, representing the lower radio inside the orbit of the planet and the largest radio to Earth orbit.
is said that a planet is at inferior conjunction when the planet is at its farthest from Earth. In the vicinity of a superior conjunction, an inner planet shows its face fully illuminated, but it is hard to see considering his apparent closeness to the Sun
Approaching greatest elongation east, being visible at dusk, the planet reveals a growing phase effect as the moon.
After a while, the planet is at inferior conjunction, it is said that the planet is at inferior conjunction when the planet is in place closest to the Earth. At inferior conjunction the planet can not be observed both for its proximity to the Sun and the small lighted portion, as directed toward Earth, its dark side. Subsequently, the planet reaches its greatest elongation west, being the planet visible in the vicinity of the dawn, until finally found a new superior conjunction.

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OTHER ASPECTS OF THE ECLIPSE OF THE SUN.

If the moon is at an angular distance less than 15 ° 21 of the node will be a partial solar eclipse this type of eclipse the moon does not touch anywhere on the Earth's surface and occurs at high latitudes (North or south). All partial eclipse takes place in two contacts. The first contact is the moment of contact between the solar and lunar discs, marking the beginning of the phenomenon. Following the progress of the moon, we reached the middle of the eclipse, which motion covers a larger fraction of the solar disk. From this point the Moon begins to leave until the last contact, the end of partial eclipse.
If the new moon is between 9 º 11 º 50'y 55'del node, the umbra will reach the Earth, resulting in an annular solar eclipse, the moon is here at the apogee and the Earth at perihelion, then the umbra is remains at 39,400 km, the center of the Earth and creates a negative or antiumbra umbra. Image of the Moon appears smaller than the Sun showing silhouettes on the bright solar photosphere. This type of eclipse has four contacts. There is a partial phase which will produce the first contact, or moment that you first touch both discs. Gradually, for an hour and a half, the solar disk will hide until the second contact occurs: when the lunar disk completely enters the solar surface. Starts central or annular phase, culminating in the middle of the event. Subsequently reversed with a third contact processes or end of the fourth annular contact or view the eclipse. Outside the annular area the observer located in the shadows, sees the phenomenon as partial. When
the new moon is less than 9 ° 55'del node and the perigee, while the Earth at aphelion, the umbra intersects the Earth producing a total solar eclipse shadow cones produce a sweep on the surface Earth called path of totality, from which the phenomenon is seen as total, out of the umbra the event is seen as partial. Total eclipses have four contacts. In the first contact both discs are played but before reaching the second contact, the ambient light changes dramatically and atmospheric parameters change. At the instant of second contact occurs diamond ring, a glow that the effect of radiation is place at the point where the photosphere disappears.

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retrogradation.

Thanks to the laws of Kepler solved the problem of the curious movement of the planets called retrogradation.
By observing the motion of a planet in the sky, is moving from West to East. However, the movement stops and often reverses the planet in an east-west, so that retraces path of the movement to stop this movement and then resume it at a West-East. This is a perspective effect due to the relative positions of the Earth and the planets on the starry background. Mechanism
a solar eclipse: One of the biggest matches of Nature: the Sun and Moon appear in the sky with the same apparent size as seen from Earth. The Moon has a diameter of 3,475 km is 400 times smaller than the Sun (1.392 million km), indicating that it is 400 times away. This condition allows the moon to cover the solar disk producing the total solar eclipse taking place for solar eclipses must be an alignment is in order, Sun-Moon-Earth, which happens every month at new moon if plans for lunar and terrestrial orbits coincide, but as the moon's orbit is inclined 5 degrees from to the ecliptic and is located sometimes above and other below the plane. Both planes, ecliptic and lunar, intersect at two points, called nodes, which are not fixed, and the moon passes twice a month. These points are the only ones that can produce eclipses.
during the solar eclipse, the moon casts a shadow on the earth's surface. These shades are composed of two distinct areas, the penumbra or outer shadow and inner shadow or umbra.

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consequences of the laws of Kepler.

According to 1 st Law, as the planets orbit the Sun ellipses and meet in one focus, distance the planet from the Sun varies, with the minimum distance when the planet is at perihelion and the maximum distance when the planet and is in line afelio.La ranging from perihelion to aphelion is called the apsidal line.
ellipses of the planets have low eccentricity (maximum 0.247 for Pluto), ie, their orbits are almost circulares.Los planets orbits travel in the forward direction (counter-clockwise to an observer in the northern hemisphere).
According to the 2 nd Law, the speed of the planet is not uniform, being greater at perihelion than at aphelion, as the distance from the Sun in the first minor in the second. Ie, "that in time equal, the ellipse arcs are traversed by a planet, the greater the closer the planet is the sun. "This difference in speed, and later was shown by Newton, is due to the attraction of the mass of the Sun exerts on the mass the planet, which being the planet next to the sun increases the attractiveness and its speed is greater.
According to the 3 rd Law, it follows that the average speed with which roam the orbits of the planets is much smaller, the farther apart the Sun's planets
Kepler's three laws, also marks the orbits of satellites around their planets.