Dimensiones del cósmicas Unidad Astronómica (U.A.): Distancia promedio Tierra - Sol = ~ 150*106 Km. Es de utilidad a escala del Sistema Solar Año Luz (A:L.): Distancia que recorre la Luz en 1 año a ~ 300.000 Km/seg. (= 9.5*1012 Km = 6.3*106 U.A.) Es de utilidad a escala del Universo. Punto de vista normal: Sistema de 3 dimensiones: Largo, Ancho y Profundidad. Punto de vista del Universo: Sistema de 4 dimensiones: Largo, Ancho, Profundidad y Tiempo. El universo que observamos desde la Tierra es aquel que se revela a través de la radiación electromagnética que nos llega. Debido a que esta radiación viaja a una velocidad finita (velocidad de la Luz), cuando observamos el universo estamos viendo hacia el pasado. Organización: Unidad Básica: Estrella (Reactor Elemental. Sintetiza elementos químicos y emite una gran cantidad de energía). Galaxia: Acumulación de estrellas (~ 108 - 1012 estrellas) Universo Isla: Acumulación de galaxias. Universo: Acumulación de Universos Isla.

Distancias estelares y/o cósmicas Tierra – Luna 1.28 Seg./Luz Diámetro del Sistema Solar ≈ 11 horas/Luz Sol-Alpha Centaury (estrella mas cercana) ≈ 4 Años/Luz Diámetro de la Galaxia 100,000 Años/Luz Galaxia mas cercana (Andrómeda) ≈ 2*106Años/Luz Universo observable en cualquier dirección ≈ 12*109 Años/Luz

¿El universo?

Nuestro sistema solar dentro de la galaxia Vía Láctea “Milky Way”

Origen del Sistema Solar, la Tierra y la Luna

Las Nebulosas son nubes interestelares de gas y polvo cósmico, son el lugar de nacimiento de las estrellas Las estrellas son los lugares en el universo donde se fabrican los elementos mas pesados que el H y He. DR21 in constellation Cygnus (infrared image) NASA/JPL-Caltech

Nebulosa de Orión

Formación del Sistema Solar

Origen del sistema solar a partir de una nebulosa 1. Nube de gas y polvo rotando lentamente 2. Contracción gravitacional, presión alta=temperatura alta pv=nrt 3. La contracción gravitacional provoca un aumento en la velocidad de rotación 3. Los anillos de material se condensan para formar los planetas

Formación del Sistema solar: Una nebulosa de rotación lenta inicia su contracción, condensación, y a aumentar su velocidad angular. 1. Nube de gas y polvo rotando lentamente 2. Contracción gravitacional, presión alta=temperatura alta pv=nrt

colisiones y acreciones en planetas terrestres y jovianos Partículas de gas y polvo chocan y acrecionan en planetesimales 3. La contracción gravitacional provoca un aumento en la velocidad de rotación colisiones y acreciones en planetas terrestres y jovianos 4. Los anillos de material se condensan para formar los planetas

Claves observables sobre el origen de nuestro planeta 1. Los planetas internos del sistema solar son mas densos y mas pequeños 2 Los planetas externos son mas grandes y menos densos 3. Los satélites de los planetas externos, están constituidos mayormente de hielo 4. Las superficies con cráteres existen en todo nuestro sistema solar 5. Saturno tiene una densidad tan baja, que no puede ser sólido en ninguna parte del planeta

Formación de la tierra por acreción La inicial nebulosa solar consistía de polvo cósmico y hielo, con los materiales menos volátiles condensando cerca del sol y los materiales menos volátiles condensando en las partes externas del sistema solar Etapa 1. Acreción de partículas de dimensiones de centímetros Etapa 2. Colisión física a escalas de kilómetros Etapa 3. Acreción gravitacional a escalas de 10 a 100 kilómetros Etapa 4. Fusión del protoplaneta debido al calor generado por la acreción

Nuestro Sistema Solar

¿Nuestra galaxia gemela? NGC7331, spiral type galaxy similar to our own. NASA's Spitzer Space Telescope has captured these infrared images of a nearby spiral galaxy that resembles our own Milky Way. The targeted galaxy, known as NGC 7331 and sometimes referred to as our galaxy's twin, is found in the constellation Pegasus at a distance of 50 million light-years. This inclined galaxy was discovered in 1784 by William Herschel, who also discovered infrared light. The evolution of this galaxy is a story that depends significantly on the amount and distribution of gas and dust, the locations and rates of star formation, and on how the energy from star formation is recycled by the local environment. The new Spitzer images are allowing astronomers to "read" this story by dissecting the galaxy into its separate components. The image, measuring 12.6 by 8.2 arcminutes, was obtained by Spitzer's infrared array camera. It is a four-color composite of invisible light, showing emissions from wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (yellow) and 8.0 microns (red). These wavelengths are roughly 10 times longer than those seen by the human eye. The infrared light seen in this image originates from two very different sources. At shorter wavelengths (3.6 to 4.5 microns), the light comes mainly from stars, particularly ones that are older and cooler than our Sun. This starlight fades at longer wavelengths (5.8 to 8.0 microns), where instead we see the glow from clouds of interstellar dust. This dust consists mainly of a variety of carbon-based organic molecules known collectively as polycyclic aromatic hydrocarbons. Wherever these compounds are found, there will also be dust granules and gas, which provide a reservoir of raw materials for future star formation. One feature that stands out in the Spitzer image is the ring of actively forming stars that surrounds the galaxy center (yellow). This ring, with a radius of nearly 20,000 light-years, is invisible at shorter wavelengths, yet has been detected at sub-millimeter and radio wavelengths. It is made up in large part of polycyclic aromatic hydrocarbons. Spitzer measurements suggest that the ring contains enough gas to produce four billion stars like the Sun. Three other galaxies are seen below NGC 7331, all about 10 times farther away. From left to right are NGC 7336, NGC 7335 and NGC 7337. The blue dots scattered throughout the images are foreground stars in the Milky Way; the red ones are galaxies that are even more distant. The Spitzer observations of NGC 7331 are part of a large 500-hour science project, known as the Spitzer Infrared Nearby Galaxy Survey, which will comprehensively study 75 nearby galaxies with infrared imaging and spectroscopy. NGC 7331 NASA/JPL-Caltech/STScI ¿Nuestra galaxia gemela?

Sol (nuestro sol) Extreme Ultraviolet Imaging Telescope (EIT) image of a huge, handle-shaped prominence taken on Sept. 14,1999 taken in the 304 angstrom wavelength - Prominences are huge clouds of relatively cool dense plasma suspended in the Sun's hot, thin corona. At times, they can erupt, escaping the Sun's atmosphere. Emission in this spectral line shows the upper chromosphere at a temperature of about 60,000 degrees K. Every feature in the image traces magnetic field structure. The hottest areas appear almost white, while the darker red areas indicate cooler temperatures. SOHO is a project of international cooperation between ESA and NASA. See the SOHO web page at http://sohowww.nascom.nasa.gov for more details. SOHO/Extreme Ultraviolet Imaging Telescope (EIT) consortium

El sistema solar This artist's concept depicts a distant hypothetical solar system, similar in age to our own. Looking inward from the system's outer fringes, a ring of dusty debris can be seen, and within it, planets circling a star the size of our Sun. This debris is all that remains of the planet-forming disk from which the planets evolved. Planets are formed when dusty material in a large disk surrounding a young star clumps together. Leftover material is eventually blown out by solar wind or pushed out by gravitational interactions with planets. Billions of years later, only an outer disk of debris remains. These outer debris disks are too faint to be imaged by visible-light telescopes. They are washed out by the glare of the Sun. However, NASA's Spitzer Space Telescope can detect their heat, or excess thermal emission, in infrared light. This allows astronomers to study the aftermath of planet building in distant solar systems like our own.

El sistema solar Se condenso de una nebulosa solar hace aproximadamente 5500 millones de años Contiene Sol, planetas, asteroides, cometas y polvo. Dos principales tipos de planetas Terrestres Jovianos

Planetas Terrestres Son pequeños y rocosos Compuestos por Oxigeno, Silicio, Aluminio, Calcio, Hierro, Magnesio Mercurio Venus Tierra Marte

Planetas Terrestres: Mercurio, Venus, Tierra y Marte Rocosos (silicatos) parte externa (corteza y manto) Fe-Ni metálico en las partes internas (núcleos). Los silicatos están compuestos por (SiO2) óxidos de otros metales. Silicatos comunes: Olivino: (Mg,Fe)SiO4 Piroxeno: (Mg,Ca,Fe)2Si2O6 feldespato (e.g., (Na,K)AlSi3O8) Mica (e.g., biotita K(Mg,Fe)3AlSi3O10(OH)). Hidden behind a shroud of dust in the constellation Cygnus is an exceptionally bright source of radio emission called DR21. Visible light images reveal no trace of what is happening in this region because of heavy dust obscuration. In fact, visible light is attenuated in DR21 by a factor of more than 10,000,000,000,000,000,000,000,000,000, 000,000,000,000 (ten thousand trillion heptillion). New images from NASA's Spitzer Space Telescope allow us to peek behind the cosmic veil and pinpoint one of the most massive natal stars yet seen in our Milky Way galaxy. The never-before-seen star is 100,000 times as bright as the Sun. Also revealed for the first time is a powerful outflow of hot gas emanating from this star and bursting through a giant molecular cloud. This image shows a 24-micron image mosaic, obtained with the Multiband Imaging Photometer aboard Spitzer (MIPS). This image maps the cooler infrared emission from interstellar dust found throughout the interstellar medium. The DR21 complex is clearly seen near the center of the strip, which covers about twice the area of the IRAC image. Perhaps the most fascinating feature in this image is a long and shadowy linear filament extending towards the 10 o'clock position of DR21. This jet of cold and dense gas, nearly 50 light-years in extent, appears in silhouette against a warmer background. This filament is too long and massive to be a stellar jet and may have formed from a pre-existing molecular cloud core sculpted by DR21's strong winds. Regardless of its true nature, this jet and the numerous other arcs and wisps of cool dust signify the interstellar turbulence normally unseen by the human eye.

Mercurio This is a mosaic of images taken of Mercury taken from 125,000 miles away. The tiny, brightly rayed crater (just below center top) was the first recognizable feature on the planet's surface and was named in memory of astronomer Gerard Kuiper, a Mariner 10 team member. The Mariner 10 spacecraft was launched in 1974. The spacecraft took images of Venus in February 1974 on the way to three encounters with Mercury in March and September 1974 and March 1975. The spacecraft took more than 7,000 images of Mercury, Venus, the Earth and the Moon during its mission. The Mariner 10 Mission was managed by the Jet Propulsion Laboratory for NASA's Office of Space Science in Washington, D.C. Davies, M. E., S. E. Dwornik, D. E. Gault, and R. G. Strom, Atlas of Mercury, NASA SP-423 (1978).

Venus

Earthrise on the Moon Planeta tierra

Marte NASA and the Hubble Heritage Team Frosty white water ice clouds and swirling orange dust storms above a vivid rusty landscape reveal Mars as a dynamic planet in this sharpest view ever obtained by an Earth-based telescope. NASA's Earth-orbiting Hubble Space Telescope took the picture on June 26, when Mars was approximately 43 million miles (68 million km) from Earth -- the closest Mars has ever been to Earth since 1988. Hubble can see details as small as 10 miles (16 km) across. The colors have been carefully balanced to give a realistic view of Mars' hues as they might appear through a telescope. Especially striking is the large amount of seasonal dust storm activity seen in this image. One large storm system is churning high above the northern polar cap [top of image], and a smaller dust storm cloud can be seen nearby. Another large dust storm is spilling out of the giant Hellas impact basin in the Southern Hemisphere [lower right]. Hubble has observed Mars before, but never in such detail. The biennial close approaches of Mars and Earth are not all the same. Mars' orbit around the Sun is markedly elliptical; the close approaches to Earth can range from 35 million to 63 million miles. Astronomers are interested in studying the changeable surface and weather conditions on Mars, in part, to help plan for a pair of NASA missions to land rovers on the planet's surface in 2004. The Mars opposition of 2001 serves as a prelude for 2003 when Mars and Earth will come within 35 million miles of each other, the closest since 1924 and not to be matched until 2287. Marte NASA and the Hubble Heritage Team

Planetas Jovianos Son grandes y gaseosos Compuestos mayormente por H y He Júpiter Saturno Urano Neptuno De esta lista se excluye a Plutón “Pluto” debido a que ya no es considerado planeta

Jupiter y Io NASA/JPL/University of Arizona Jupiter's four largest satellites, including Io, the golden ornament in front of Jupiter in this image from NASA's Cassini spacecraft, have fascinated Earthlings ever since Galileo Galilei discovered them in 1610 in one of his first astronomical uses of the telescope. Images from Cassini that will be released over the next several days capture each of the four Galilean satellites in their orbits around the giant planet. This true-color composite frame, made from narrow angle images taken on Dec. 12, 2000, captures Io and its shadow in transit against the disk of Jupiter. The distance of the spacecraft from Jupiter was 19.5 million kilometers (12.1 million miles). The image scale is 117 kilometers (73 miles) per pixel. The entire body of Io, about the size of Earth's Moon, is periodically flexed as it speeds around Jupiter and feels, as a result of its non-circular orbit, the periodically changing gravitational pull of the planet. The heat arising in Io's interior from this continual flexure makes it the most volcanically active body in the solar system, with more than 100 active volcanoes. The white and reddish colors on its surface are due to the presence of different sulfurous materials. The black areas are silicate rocks. Cassini is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini mission for NASA's Office of Space Science, Washington, D.C. Jupiter y Io NASA/JPL/University of Arizona

Saturno NASA/JPL/GSFC/Ames The varying temperatures of Saturn's rings are depicted here in this false-color image from the Cassini spacecraft. This image represents the most detailed look to date at the temperature of Saturn's rings. The image was made from data taken by Cassini's composite infrared spectrometer instrument. Red represents temperatures of about 110 Kelvin (-261 degrees Fahrenheit), and blue 70 Kelvin (-333 degrees Fahrenheit). Green is equivalent to 90 Kelvin (-298 degrees Fahrenheit). Water freezes at 273 Kelvin (32 degrees Fahrenheit). The spatial resolution of the ring portion of the image is 200 kilometers (124 miles). The data show that the opaque region of the rings, like the outer A ring (on the far right) and the middle B ring, are cooler, while more transparent sections, like the Cassini Division (in red just inside the A ring) or the inner C ring (shown in yellow and red), are relatively warmer. The temperature data were taken on July 1, 2004, of the unlit side of the rings. In order to show the full breadth of the rings, a strip of temperature data was mapped onto a picture of the lit side of the rings taken with the Cassini narrow angle camera on May 11, 2004, a little over a month before Saturn orbit insertion. Cassini is too close to the planet and hence no pictures of the unlit side of the rings are available, so the temperature data were mapped onto a picture of the lit side of rings. Saturn is overexposed and pure white in this picture. Saturn's moon Enceladus is visible below the rings, toward the center The original picture and caption are available at PIA05410. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA's Science and Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The Composite Infrared Spectrometer team is based at NASA's Goddard Space Flight Center, Greenbelt, Md. For more information about the Cassini-Huygens mission, visit http://saturn.jpl.nasa.gov and the instrument team's home page, http://cirs.gsfc.nasa.gov/ . Saturno NASA/JPL/GSFC/Ames

L a primera foto a color de la superficie de Titan’ Enero 14, 2005 Hielo de agua e hidrocarburos This image was returned, January 14, 2005, by the European Space Agency's Huygens probe during its successful descent to land on Titan. This is the colored view, following processing to add reflection spectra data, and gives a better indication of the actual color of the surface. Initially thought to be rocks or ice blocks, they are more pebble-sized. The two rock-like objects just below the middle of the image are about 15 centimeters (about 6 inches) (left) and 4 centimeters (about 1.5 inches) (center) across respectively, at a distance of about 85 centimeters (about 33 inches) from Huygens. The surface is darker than originally expected, consisting of a mixture of water and hydrocarbon ice. There is also evidence of erosion at the base of these objects, indicating possible fluvial activity. The image was taken with the Descent Imager/Spectral Radiometer, one of two NASA instruments on the probe. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The Descent Imager/Spectral team is based at the University of Arizona, Tucson, Ariz. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm. ESA/NASA/Univ. of Arizona

Urano Kenneth Seidelmann, U.S. Naval Observatory, and NASA A recent Hubble Space Telescope view reveals Uranus surrounded by its four major rings and by 10 of its 17 known satellites. This false-color image was generated by Erich Karkoschka using data taken on August 8, 1998, with Hubble's Near Infrared Camera and Multi-Object Spectrometer. Hubble recently found about 20 clouds - nearly as many clouds on Uranus as the previous total in the history of modern observations. The Wide Field/Planetary Camera 2 was developed by the Jet Propulsion Laboratory and managed by the Goddard Spaced Flight Center for NASA's Office of Space Science. This image and other images and data received from the Hubble Space Telescope are posted on the World Wide Web on the Space Telescope Science Institute home page at URL http://oposite.stsci.edu/pubinfo/ Kenneth Seidelmann, U.S. Naval Observatory, and NASA

Neptuno

The never-before-seen surface of the distant planet Pluto is resolved in these NASA Hubble Space Telescope pictures, taken with the European Space Agency's (ESA) Faint Object Camera (FOC) aboard Hubble. Discovered in 1930, Pluto has always appeared as nothing more than a dot of light in even the largest Earth-based telescopes because Pluto's disk is much smaller than can be resolved from beneath the Earth's turbulent atmosphere. Pluto is 2/3 the size of Earth's Moon but 12,000 times farther away. Viewing surface detail is as difficult as trying to read the printing on a golf ball located thirty-three miles away! Hubble imaged nearly the entire surface of Pluto, as it rotated through its 6.4-day period, in late June and early July 1994. These images, which were made in blue light, show that Pluto is an unusually complex object, with more large-scale contrast than any planet, except Earth. Pluto itself probably shows even more contrast and perhaps sharper boundaries between light and dark areas than is shown here, but Hubble's resolution (just like early telescopic views of Mars) tends to blur edges and blend together small features sitting inside larger ones. The two smaller inset pictures at the top are actual images from Hubble. North is up. Each square pixel (picture element) is more than 100 miles across. At this resolution, Hubble discerns roughly 12 major "regions" where the surface is either bright or dark. The larger images (bottom) are from a global map constructed through computer image processing performed on the Hubble data. The tile pattern is an artifact of the image enhancement technique. Opposite hemispheres of Pluto are seen in these two views. Some of the variations across Pluto's surface may be caused by topographic features such as basins, or fresh impact craters. However, most of the surface features unveiled by Hubble, including the prominent northern polar cap, are likely produced by the complex distribution of frosts that migrate across Pluto's surface with its orbital and seasonal cycles and chemical byproducts deposited out of Pluto's nitrogen-methane atmosphere. The picture was taken in blue light when Pluto was at a distance of 3 billion miles from Earth. This image and other images and data received from the Hubble Space Telescope are posted on the World Wide Web on the Space Telescope Science Institute home page at URL http://oposite.stsci.edu/pubinfo/ Alan Stern (Southwest Research Institute), Marc Buie (Lowell Observatory), NASA and ESA

Earthrise on the Moon La tierra desde la luna

Datos de la Luna Gran masa con respecto a la tierra Gran momento angular del sistema tierra-luna La luna esta empobrecida en elementos volátiles y hierro La tierra y la luna tienen cocientes isotópicos de oxigeno similares La luna alguna ves estuvo completamente fundida (océano de magma)

Hipótesis sobre el origen de la luna Captura de una orbita heliocéntrica orbita independiente Co-acreción Fisión de la tierra con rotación muy rápida Expulsión por Colisión Captura no integrativa

El Programa Apolo Resolver el origen de la luna fue el objetivo científico Se tuvieron como resultado grandes avances tecnológicos

Hipótesis de la expulsión colisional Explicación La tierra fue impactada por un objeto de las dimensiones de Marte El manto rocoso del objeto y la Tierra fueron vaporizados parcialmente y fueron expulsados hacia una orbita alrededor de la tierra Polvo y vapor coalecen para formar la luna

0 segundos Sandia National Laboratories

403 segundos Sandia National Laboratories

804 segundos Sandia National Laboratories

1204 segundos Sandia National Laboratories

1600 segundos Sandia National Laboratories

2003 segundos Sandia National Laboratories

Meteoritos Fragmentos de cuerpos formados tempranamente llamados planetesimales 3 principales tipos de meteoritos Condritos material del sistema solar inicial Rocosos Ferrosos Todos tienen la misma edad – del sistema solar inicial 4500 millones de años

Meteoritos Condritos Condrules Allende

Meteorito Ferroso – Canyon Diablo

Textura Widmanstätten de aleaciones de Fe-Ni

Resumen El Universo tiene aprox. 14 mil años. El Sistema solar consiste de 9 planetas, 4 terrestres y 5 Jovianos, que orbitan alrededor del sol (orbita heliocéntrica). El sol y los plantas se formaron por acreción de partículas y gases hace 4500 millones de años. La luna se formo por colisión con la Tierra de un objeto del tamaño de Marte (hipótesis de eyección colisional)

Resumen Muchos procesos naturales, tales como el origen de la tierra y la luna, no pueden ser observados directamente y deben ser inferidos de observaciones indirectas, mediciones y cálculos. Ejemplo: El origen y la historia temprana de la tierra son inferidos a partir del análisis de meteoritos, de la luna y de otros planetas.