Monday, December 29, 2008

NGC 6960: The Witch's Broom Nebula


Credit & Copyright: Adam Block, Mount Lemmon SkyCenter, Univ. Arizona

Explanation: Ten thousand years ago, before the dawn of recorded human history, a new light must suddenly have appeared in the night sky and faded after a few weeks. Today we know this light was an exploding star and record the colorful expanding cloud as the Veil Nebula. Pictured above is the west end of the Veil Nebula known technically as NGC 6960 but less formally as the Witch's Broom Nebula. The expanding debris cloud gains its colors by sweeping up and exciting existing nearby gas. The supernova remnant lies about 1400 light-years away towards the constellation of Cygnus. This Witch's Broom actually spans over three times the angular size of the full Moon. The bright star 52 Cygni is visible with the unaided eye from a dark location but unrelated to the ancient supernova.

31 Million Miles from Planet Earth


Univ. Maryland, EPOCh/DIXI Science Teams

Explanation: On July 4th, 2005, the Deep Impact spacecraft directed a probe to impact the nucleus of Comet Tempel 1. Still cruising through the solar system, earlier this year the robotic spacecraft looked back to record a series of images of its home world 31 million miles (50 million kilometers) away. In a sequence from top left to bottom right, these four frames from the video show a rotating Earth. They combine visible and near-infrared image data with enough resolution and contrast to see clouds, oceans, and continents. They also follow a remarkable transit of Earth by its large, natural satellite, the Moon. The Moon's orbital motion carries it across the field of view from left to right. Imaging the Earth from this distant perspective allows astronomers to connect overall variations in brightness at different wavelengths with planetary features. The observations will aid in the search for earthlike planets in other planetary systems.

Mirach's Ghost


Credit & Copyright: Anthony Ayiomamitis (TWAN)

Explanation: As far as ghosts go, Mirach's Ghost isn't really that scary. In fact, Mirach's Ghost is just a faint, fuzzy galaxy, well known to astronomers, that happens to be seen nearly along the line-of-sight to Mirach, a bright star. Centered in this star field, Mirach is also called Beta Andromedae. About 200 light-years distant, Mirach is a red giant star, cooler than the Sun but much larger and so intrinsically much brighter than our parent star. In most telescopic views, glare and diffraction spikes tend to hide things that lie near Mirach and make the faint, fuzzy galaxy look like a ghostly internal reflection of the almost overwhelming starlight. Still, appearing in this sharp image just above and to the right, Mirach's Ghost is cataloged as galaxy NGC 404 and is estimated to be some 10 million light-years away.

Thackeray's Globules



Credit: Hubble Heritage Team (STScI/AURA), NASA

Explanation: Rich star fields and glowing hydrogen gas silhouette dense, opaque clouds of interstellar gas and dust in this Hubble Space Telescope close-up of IC 2944, a bright star forming region in Centaurus, 5,900 light-years away. The largest of these dark globules, first spotted by South African astronomer A. D. Thackeray in 1950, is likely two separate but overlapping clouds, each more than one light-year wide. Combined the clouds contain material equivalent to about 15 times the mass of the Sun, but will they actually collapse to form massive stars? Along with other data, the sharp Hubble images indicate that Thackeray's globules are fractured and churning as a result of intense ultraviolet radiation from young, hot stars already energizing and heating the bright emission nebula. These and similar dark globules known to be associated with other star forming regions may ultimately be dissipated by their hostile environment -- like cosmic lumps of butter in a hot frying pan.

NGC 1569: Starburst in a Dwarf Irregular Galaxy



Credit: NASA, ESA, Hubble Heritage (STScI/AURA)

Explanation: Grand spiral galaxies often seem to get all the glory, flaunting their young, bright, blue star clusters in beautiful, symmetric spiral arms. But small, irregular galaxies form stars too. In fact, as pictured here, dwarf galaxy NGC 1569 is apparently undergoing a burst of star forming activity, thought to have begun over 25 million years ago. The resulting turbulent environment is fed by supernova explosions as the cosmic detonations spew out material and trigger further star formation. Two massive star clusters - youthful counterparts to globular star clusters in our own spiral Milky Way galaxy - are seen left of center in the gorgeous Hubble Space Telescope image. The above picture spans about 8,000 light-years across NGC 1569. A mere 11 million light-years distant, this relatively close starburst galaxy offers astronomers an excellent opportunity to study stellar populations in rapidly evolving galaxies. NGC 1569 lies in the long-necked constellation Camelopardalis.

The Small Cloud of Magellan


Credit & Copyright: Josch Hambsch, Robert Gendler

Explanation: Portuguese navigator Ferdinand Magellan and his crew had plenty of time to study the southern sky during the first circumnavigation of planet Earth. As a result, two celestial wonders easily visible for southern hemisphere skygazers are known as the Clouds of Magellan. These cosmic clouds are now understood to be dwarf irregular galaxies, satellites of our larger spiral Milky Way Galaxy. The Small Magellanic Cloud pictured above actually spans 15,000 light-years or so and contains several hundred million stars. About 210,000 light-years distant in the constellation Tucana, it is the fourth closest of the Milky Way's known satellite galaxies, after the Canis Major and Sagittarius Dwarf galaxies and the Large Magellanic Cloud. This gorgeous view also includes two foreground globular star clusters NGC 362 (top left) and 47 Tucanae. Spectacular 47 Tucanae is a mere 13,000 light-years away and seen here to the right of the Small Magellanic Cloud.

NGC 7023: The Iris Nebula


Image Credit & Copyright: Jim Misti (acquisition), Robert Gendler (processing)

Explanation: Like delicate cosmic petals, these clouds of interstellar dust and gas have blossomed 1,300 light-years away in the fertile star fields of the constellation Cepheus. Sometimes called the Iris Nebula and dutifully cataloged as NGC 7023, this is not the only nebula in the sky to evoke the imagery of flowers. Still, the beautiful digital image shows off the Iris Nebula's range of colors and symmetries in impressive detail. Within the Iris, dusty nebular material surrounds a massive, hot, young star in its formative years. Central filaments of cosmic dust glow with a reddish photoluminesence as some dust grains effectively convert the star's invisible ultraviolet radiation to visible red light. Yet the dominant color of the nebula is blue, characteristic of dust grains reflecting starlight. Dark, obscuring clouds of dust and cold molecular gas are also present and can lead the eye to see other convoluted and fantastic shapes. Infrared observations indicate that this nebula may contain complex carbon molecules known as PAHs. As shown here, the Iris Nebula is about 6 light-years across.

Himalayan Horizon From Space


Credit: Expedition 1, ISS, EOL NASA

Explanation: This stunning aerial view shows the rugged snow covered peaks of a Himalayan mountain range in Nepal. The seventh-highest peak on the planet, Dhaulagiri, is the high point on the horizon at the left while in the foreground lies the southern Tibetan Plateau of China. But, contrary to appearances, this picture wasn't taken from an airliner cruising at 30,000 feet. Instead it was taken with a 35mm camera and telephoto lens by the Expedition 1 crew aboard the International Space Station -- orbiting 200 nautical miles above the Earth. The Himalayan mountains were created by crustal plate tectonics on planet Earth some 70 million years ago, as the Indian plate began a collision with the Eurasian plate. Himalayan uplift still continues today at a rate of a few millimeters per year.

G21.5-0.9: A Supernova's Cosmic Shell



Credit: Heather Matheson & Samar Safi-Harb (Univ. Manitoba), CXC, NASA

Explanation: The picture is lovely, but this pretty cosmic shell was produced by almost unbelievable violence - created when a star with nearly 20 times the mass of the sun blasted away its outer layers in a spectacular supernova explosion. As the expanding debris cloud swept through surrounding interstellar material, shock waves heated the gas causing the supernova remnant to glow in x-rays. In fact, it is possible that all supernova explosions create similar shells, some brighter than others. Cataloged as G21.5-0.9, this shell supernova remnant is relatively faint, requiring about 150 hours of x-ray data from the orbiting Chandra Observatory to create this false-color image. G21.5-0.9 is about 20,000 light-years distant in the constellation Scutum and measures about 30 light-years across. Based on the remnant's size, astronomers estimate that light from the original stellar explosion first reached Earth several thousand years ago.

The Hercules Cluster of Galaxies



Credit & Copyright: Jim Misti (Misti Mountain Observatory)

Explanation: These are galaxies of the Hercules Cluster, an archipelago of "island universes" a mere 650 million light-years distant. This cluster is loaded with gas and dust rich, star forming, spiral galaxies but has relatively few elliptical galaxies, which lack gas and dust and the associated newborn stars. Colors in the composite image show the star forming galaxies with a blue tint and ellipticals with a slightly yellowish cast. In this cosmic vista many galaxies seem to be colliding or merging while others seem distorted - clear evidence that cluster galaxies commonly interact. Over time, the galaxy interactions are likely to affect the the content of the cluster itself. Researchers believe that the Hercules Cluster is significantly similar to young galaxy clusters in the distant, early Universe and that exploring galaxy types and their interactions in nearby Hercules will help unravel the threads of galaxy andcluster evolution.

M51: Cosmic Whirlpool



Credit: S. Beckwith (STScI) Hubble Heritage Team, (STScI/AURA), ESA, NASA

Explanation: Follow the handle of the Big Dipper away from the dipper's bowl, until you get to the handle's last bright star. Then, just slide your telescope a little south and west and you might find this stunning pair of interacting galaxies, the 51st entry in Charles Messier's famous catalog. Perhaps the original spiral nebula, the large galaxy with well defined spiral structure is also cataloged as NGC 5194. Its spiral arms and dust lanes clearly sweep in front of its companion galaxy (right), NGC 5195. The pair are about 31 million light-years distant and officially lie within the boundaries of the small constellation Canes Venatici. Though M51 looks faint and fuzzy in small, earthbound telescopes, this sharpest ever picture of M51 was made in January 2005 with the Advanced Camera for Surveys on board the Hubble Space Telescope.

La Superba



Credit & Copyright: Processing - Noel Carboni, Imaging - Greg Parker, New Forest Observatory

Explanation: Y Canum Venaticorum (Y CVn) is a very rare star in planet Earth's night sky. It's also very red, exhibiting such a remarkable spectrum of light, 19th century astronomer Angelo Secchi dubbed it La Superba. Located 710 light-years away in northern constellation Canes Venatici (the Hunting Dogs), the star varies in brightness over a period of about half a year. Near maximum, it becomes just bright enough to see with the unaided eye, but the star's beautiful red hue is easy to see in binoculars or a small telescope. In fact, La Superba is among the brightest of the carbon stars - cool, highly evolved red giant stars with exceptional abundances of carbon. The carbon is created by helium fusion near the stellar core and dredged up into the stars' outer layers. The resulting overabundance of simple carbon molecules (like CO, CN, C2) in the atmospheres of carbon stars strongly absorbs bands of bluer light and gives these stars a deep red color. La Superba is losing its carbon-rich atmosphere into the surrounding interstellar material through a strong stellar wind, and could be near the beginning of a transition to a planetary nebula phase.

Milky Way Illustrated



Illustration Credit & Copyright: Mark Garlick (Space-art)

Explanation: What does our Milky Way Galaxy look like from afar? Since we are stuck inside, and since opaque dust truncates our view in visible light, nobody knows for sure. Drawn above, however, is a good guess based on many different types of observations. In the Milky Way's center is a very bright core region centered on a large black hole. The Milky Way's bright central bulge is now thought to be an asymmetrical bar of relatively old and red stars. The outer regions are where the spiral arms are found, dominated in appearance by open clusters of young, bright, blue stars, by red emission nebula, and by dark dust. The spiral arms reside in a disk dominated in mass by relatively dim stars and loose gas composed mostly of hydrogen. What is not depicted is a huge spherical halo of invisible dark matter that dominates the mass of the Milky Way as well as the motions of stars away from the center.

The Pleiades Star Cluster



Credit and Copyright: Matthew T. Russell

Explanation: Perhaps the most famous star cluster on the sky, the Pleiades can be seen without binoculars from even the depths of a light-polluted city. Also known as the Seven Sisters and M45, the Pleiades is one of the brightest and closest open clusters. The Pleiades contains over 3000 stars, is about 400 light years away, and only 13 light years across. Quite evident in the above photograph are the blue reflection nebulae that surround the brighter cluster stars. Low mass, faint, brown dwarfs have also been found in the Pleiades. (Editors' note: The prominent diffraction spikes are caused by the telescope itself and may be either distracting or provide aesthetic enhancement, depending on your point of view.)

Welcome to Planet Earth


Credit: Apollo 17 Crew, NASA

Explanation:

Welcome to Planet Earth, the third planet from a star named the Sun. The Earth is shaped like a sphere and composed mostly of rock. Over 70 percent of the Earth's surface is water. The planet has a relatively thin atmosphere composed mostly of nitrogen and oxygen. Earth has a single large Moon that is about 1/4 of its diameter and, from the planet's surface, is seen to have almost exactly the same angular size as the Sun. With its abundance of liquid water, Earth supports a large variety of life forms, including potentially intelligent species such as dolphins and humans. Please enjoy your stay on Planet Earth.

Manicouagan Impact Crater


Credit: STS-9 Crew, NASA

Explanation: Manicouagan Crater in northern Canada is one of the oldest impact craters known. Formed about 200 million years ago, the present day terrain supports a 70-kilometer diameter hydroelectric reservoir in the telltale form of an annular lake. The crater itself has been worn away by the passing of glaciers and other erosional processes. Still, the hard rock at the impact site has preserved much of the complex impact structure and so allows scientists a leading case to help understand large impact features on Earth and other Solar System bodies. Also visible above is the vertical fin of the Space Shuttle Columbia from which the picture was taken in 1983.

Abell 2218: A Galaxy Cluster Lens


Picture Credit: NASA, HST, WFPC2, W. Couch (UNSW)

Explanation: Sometimes one of the largest concentrations of mass known can act like a lens. Almost all of the bright objects in this image are galaxies in the cluster known as Abell 2218. The cluster is so massive and so compact that it bends light from galaxies that lie behind it, causing many of them to appear as stretched out arcs. Many dim, elongated arcs are visible on this photograph. This picture was taken with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope.

July 10, 1995

A Meteoric View of Apollo 13


Picture Credit: Unknown

Explanation: Meteors, also called shooting stars, normally begin as bits of dust from the tails of comets or even small pieces chipped off asteroids. Falling toward Earth, these particles enter the atmosphere at extremely high speeds. Friction with the air heats them up and makes them glow brightly. Their rapid motion across the sky causes them to show up as bright streaks in photographs. In this picture, however, the bright streaks which appear to be meteor trails are believed to be two large pieces of the Apollo 13 spacecraft, the service and lunar modules, reentering the atmosphere.

Damage to Apollo 13



Picture Credit: NASA, Crew of Apollo 13

Explanation: In April of 1970, after an oxygen tank exploded and damaged their service module, the Apollo 13 astronauts were forced to abandon their plans to make the third manned lunar landing. The extent of the damage is revealed in this photo, taken as the crippled module was drifting away - jettisoned prior to their reentry and eventual safe splashdown. An entire panel on the right side of the module is seen to have been blown away and damage to internal structures is apparent.

Lunar Farside from Apollo 13


Picture Credit: NASA, Crew of Apollo 13

Explanation: In April of 1970, after an explosion damaged their spacecraft, the Apollo 13 astronauts were forced to abandon their plans to make the third manned lunar landing. Still, while coasting around the moon in their desperate attempt to return to earth they were able to photograph the moon's far side. The large, dark, smooth looking feature on the left in this picture is known as the "Mare Moscoviense". It was created by a lava flow filling in a large impact crater on the lunar surface. As suggested by the name, the Mare Moscoviense was first photographed by an early Soviet lunar probe.

July 7, 1995

Saturn, Rings, and Two Moons


Picture Credit: NASA, Jet Propulsion Laboratory,Voyager Project

Explanation: This image of Saturn was made by NASA's robot spacecraft Voyager 2 as it began to explore the Saturn system in 1981. Saturn's famous rings are visible along with two of its moons, Rhea and Dione which appear as faint dots in the right and lower right part of the picture. Astronomers believe that Saturn's moons play a fundamental role in sculpting its elaborate ring system.

July 6, 1995

The Night Side of Saturn


Picture Credit: NASA, Jet Propulsion Laboratory,Voyager Project

Explanation: This image of Saturn was made in November 1980 by the Voyager 1 spacecraft as it flew past the ringed gas giant planet. From a spectacular vantage point, looking back toward the inner solar system, the robot spacecraft recorded this view of the night side of Saturn casting a sharp shadow across the bright rings. No Earth based telescope could ever take a similar picture. Since Earth is closer to the sun than Saturn, only the day side of the planet is visible from the Earth.

July 5, 1995

The Firework Nebula


Picture Credit: WIYN Telescope

Explanation: The Firework Nebula, known to astronomers as "GK Per", is the result of a type of stellar explosion called a nova. In a nova, a very compact star called a white dwarf blasts away gas that had accumulated on its surface. In this case the nova occurred in the year 1901 and is called Nova Persei 1901. This nova became as bright as one of the brighter stars we see in the night sky, but then faded until only a telescope could see it. Soon astronomers could see an expanding shell of gas that eventually became this spectacular nebula. The unusual "fireworks" type feature of this nebula is still a matter of research and discussion.

July 4, 1995

The Great Nebula in Orion


Picture Credit: NASA, Hubble Space Telescope

Explanation: The Great Nebula in Orion, M42, can be found on the night sky just below and to the left of the easily identifiable belt of three stars in the popular constellation Orion. This nebula is one of the closest stellar nurseries - where young stars are being formed even now. Clumps of gas (mostly hydrogen and helium) and dust in the nebula are squeezed together by their own gravity until they collapse and form stars. Some stars we can see here partially obscured by the nebula, are only about 100,000 years old - just babies compared to the 5 billion (5,000,000,000) years of our Sun.

July 3, 1995

The Cartwheel Galaxy


Picture Credit: NASA, Hubble Space Telescope

Explanation: The Cartwheel Galaxy shows a ring that is the result of a collision between a small and a large galaxy. After a small galaxy has moved through a big galaxy - in this case one that probably resembled our own Milky Way - a star formation wave moves out from the impact point like ripples across the surface of a pond. When galaxies collide it is rare that any two stars actually collide. Gravity, however, causes density waves to move out through the galaxy which in turn triggers the formation of hot, bright young stars, producing the ring that we see in this picture.

July 2, 1995

The Hooker Telescope on Mt. Wilson


Picture Credit: Mount Wilson Observatory

Explanation: In the 1920s, pictures from the Hooker Telescope on Mt. Wilson fundamentally changed our understanding of the cosmos. Astronomer Edwin Hubble, using photographs he took with this telescope, demonstrated that the objects his contemporaries called "spiral nebulae" were actually huge systems of stars - spiral galaxies, similar to our own Milky Way galaxy but incredibly distant. Prior to Hubble's work it was argued that the spiral nebulae were mere clouds of gas and that they, along with everything else in the universe, were contained in our own galaxy. The Hooker Telescope mirror is 100 inches in diameter which is nearly the size of the mirror of the orbiting Hubble Space Telescope named in Hubble's honor. The Mount Wilson Observatory offers a "virtual walking tour" of this historic telescope.

July 1, 1995

Ida and Dactyl: Asteroid and Moon


Picture Credit: NASA, JPL, Galileo Project

Explanation: An asteroid with a moon! The robot spacecraft Galileo whose primary mission is to explore the Jupiter system, has encountered and photographed two asteroids during its long journey to Jupiter. The second asteroid it photographed, called Ida, was discovered to have a moon which appears as a small dot to the right of Ida in this picture. The tiny moon, named Dactyl, is about one mile across, while the potato shaped Ida measures about 36 miles long and 14 miles wide. Dactyl is the first moon of an asteroid ever discovered. The names Ida and Dactyl are based on characters in Greek mythology.

June 30, 1995

The Earth-Moon System


Picture Credit: NASA, JPL, Galileo Project

Explanation: A double planet? From 4 million miles away on December 16, 1992, NASA's robot spacecraft Galileo took this picture of the Earth-moon system. The bright, sunlit half of the Earth contrasts strongly with the darker subdued colors of the moon. Our moon is one of the largest moons in the solar system. It is even larger than the planet Pluto. In this picture, the Earth-moon system actually appears to be a double planet.

June 29, 1995

The Cat's Eye Nebula


Picture Credit: NASA, Hubble Space Telescope

Explanation: Three thousand light years away, a dying star throws off shells of glowing gas. This Hubble Space Telescope image reveals "The Cat's Eye Nebula" to be one of the most complex "planetary nebulae" known. In fact, the features seen in this image are so complex that astronomers suspect the visible central star may actually be a double star system. The term planetary nebula, used to describe this general class of objects, is misleading. Although these objects may appear round and planet-like in small telescopes, high resolution images reveal them to be stars surrounded by cocoons of gas blown off in the late stages of evolution.

June 28, 1995

An Ultraviolet Image of Messier 101


Picture Credit: NASA, Ultraviolet Imaging Telescope (UIT)

Explanation: This giant spiral galaxy, Messier 101 (M101), was photographed by the Ultraviolet Imaging Telescope onboard the Space Shuttle Endeavour during the Astro-2 mission (March 2 - 18, 1995). The image has been computer processed so that the colors represent the intensity of ultraviolet light. Pictures of galaxies like this one show mainly clouds of gas containing newly formed stars many times more massive than the sun, which glow strongly in ultraviolet light. In contrast, visible light pictures of galaxies tend to be dominated by the yellow and red light of older stars. Ultraviolet light, invisible to the human eye, is blocked by ozone in the atmosphere so ultraviolet pictures of celestial objects must be taken from space.

June 27, 1995

The Spiral Galaxy M100


Picture Credit: NASA, Hubble Space Telescope

Explanation: The M100 galaxy is a large spiral galaxy similar to our own Milky Way, containing over 100 billion stars. It is over 150 million light years away, so the light we see left when dinosaurs roamed the Earth. The picture was taken in 1993 with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope.

June 26, 1995

Jupiter from Voyager


June 25, 1995

Picture Credit: NASA, JPL, NSSDC, Voyager

Explanation: Imagine a hurricane that lasted for 300 years! This picture of the planet Jupiter was taken by the Voyager 1 spacecraft as it passed the planet in 1979. Jupiter, a gas giant planet with no solid surface, is the largest planet in the solar system and is made mostly of the hydrogen and helium. Clearly visible in the photo is the Great Red Spot, a giant, hurricane-like storm system that rotates with the clouds of Jupiter. It is so large three complete Earths could fit inside it. Astronomers have observed this giant storm on Jupiter for over 300 years.

The Crab Nebula and Geminga in Gamma Rays


June 24, 1995

Picture Credit: NASA, Compton Gamma Ray Observatory

Explanation: What if you could "see" in gamma-rays? If you could, these two spinning neutron stars or pulsars would be among the brightest objects in the sky. This computer processed image shows the Crab Nebula pulsar (below and right of center) and the Geminga pulsar (above and left of center) in the "light" of gamma-rays. Gamma-ray photons are more than 10,000 times more energetic than visible light photons and are blocked from the Earths's surface by the atmosphere. This image was produced by the high energy gamma-ray telescope "EGRET" on board NASA's orbiting Compton Observatory satellite.

Gamma Ray All Sky Map


June 23, 1995

Picture Credit: NASA, Compton Gamma Ray Observatory

Explanation:

What if you could "see" gamma rays? This computer processed image represents a map of the entire sky at photon energies above 100 million electron Volts. These gamma-ray photons are more than 40 million times more energetic than visible light photons and are blocked from the Earth's surface by the atmosphere. In the early 1990s NASA's Compton Gamma Ray Observatory, in orbit around the Earth, scanned the entire sky to produce this picture. A diffuse gamma-ray glow from the plane of our Milky Way Galaxy is clearly seen across the middle. The nature and even distance to some of the fainter sources remain unknown.

Earth from Apollo 17


The Earth from Apollo 17

Picture Credit: NASA, Apollo 17, NSSDC

Explanation: In 1972 Astronauts on the United States's last lunar mission, Apollo 17, took this picture looking back at the Earth on their way to the moon. The continents of Antarctica and Africa are visible below the delicate wisps of white clouds.

Supernova 1987a Aftermath


June 21 1995

Picture Credit: Hubble Space Telescope

Explanation: In 1987 a star in one of the Milky Way's satellite galaxies exploded. In 1994 the Hubble Space Telescope, in orbit around the earth, took a very detailed picture of the remnants of this explosion. This picture, above, showed unusual and unexpected rings, and astronomers are not sure how they formed.

Pleiades Star Cluster


June 20 1995

Picture Credit: Mount Wilson Observatory

Explanation:

The Pleiades star cluster, M45, is one of the brightest star clusters visible in the northern hemisphere. It consists of many bright, hot stars that were all formed at the same time within a large cloud of interstellar dust and gas. The blue haze that accompanies them is due to very fine dust which still remains and preferentially reflects the blue light from the stars.

Neutron Star Earth



June 16 1995

Explanation:

If the Earth could somehow be transformed to the ultra-high density of a neutron star,it might appear as it does in the above computer generated figure. Due to the very strong gravitational field, the neutron star distorts light from the background sky greatly. If you look closely, two images of the constellation Orion are visible. The gravity of this particular neutron star is so great that no part of the neutron star is blocked from view - light is pulled around by gravity even from the back of the neutron star.

Dwarf stars emit powerful pulse


This image shows what it might look like standing on the surface of a planet orbiting a brown dwarf star. An alien moon can also be seen in the sky. The brown dwarf gives off such feeble visible light it is difficult to see any of the landscape except for the reflection in the water.Brown dwarfs are a type of "failed" star.(Artist View)

Friday, 20 April 2007

The brown dwarfs are behaving like an altogether different and exotic cosmic object called a pulsar.Pulsars are rotating neutron stars that emit a flashing radio signal.
When the rotating beams sweep Earth, astronomers detect the radio pulse, which has been likened to the rotating beacon of a lighthouse.Pulsars are created when a massive star explodes in a supernova and its core collapses into a rapidly spinning neutron star.Brown dwarfs, on the other hand, are stellar also-rans which lack the necessary mass to kick-start nuclear fusion reactions in their cores.Greg Hallinan from the National University of Ireland in Galway and his colleagues used the Very Large Array radio telescope in New Mexico to observe a very cool, rapidly rotating brown dwarf called TVLM 513-46546.

40-year-old problem:

A class of "failed" star called a brown dwarf emits beams of radiation that are thousands of times brighter than any released by the Sun.A bright flash from the brown dwarf was observed roughly every two hours.All the planets with a magnetic field, including Earth, have bright radio emission from their magnetic polar regions.Brown dwarfs are thought to generate their emission in a similar way to pulsars. But here, the emission is many times brighter than that from planets. The radio waves are produced above the object's magnetic poles.
This radio emission requires these brown dwarfs to possess magnetic fields as powerful as those detected at the most magnetically active stars.The periodic pulses detected from brown dwarfs are very similar to those observed from pulsars. But the whole system is on a much slower and smaller scale, so it is easier for astronomers to decipher what is going on.

Link made?:

How pulsars produce their radiation has been a problem in astrophysics for 40 years.
This is because we have little understanding of how hot, electrified gas, or plasma, behaves in the extreme conditions present at a pulsar.Brown dwarfs are now the second class of stellar object known to produce persistent levels of extremely bright, "coherent" radiation.Moreover, this radio signal manifests itself as periodic pulses. However, in the case of brown dwarfs, both the source conditions and the emission mechanism are reasonably well understood.For some time, scientists have wondered if there were similarities between this type of emission and the periodic radio beams from pulsars. Observations of TVLM 513-46546 could provide the first direct evidence for such a link.Dr Hallinan said: "Our research shows that these objects can be fascinating and dynamic systems, and may be the key to unlocking this long-standing mystery of how pulsars produce radio emissions.
"It looks like brown dwarfs are the missing step between the radio emissions we see generated at Jupiter and those we observe from pulsars".

The National University of Ireland astrophysicist presented details of his work at the Royal Astronomical Society's National Astronomy Meeting in Preston.

Sunday, December 28, 2008

Neutron Star/Quark Star Interior



Quark Star:


A quark star or strange star is a hypothetical type of exotic star composed of quark matter, or strange matter. These are ultra-dense phases of degenerate matter theorized to form inside particularly massive neutron stars.It is theorized that when the neutron-degenerate matter which makes up a neutron star is put under sufficient pressure due to the star's gravity, the individual neutrons break down into their constituent quarks, up quarks and down quarks. Some of these quarks may then become strange quarks and form strange matter. The star then becomes known as a "quark star" or "strange star", similar to a single gigantic hadron (but bound by gravity rather than the strong force). Quark matter/strange matter is one candidate for the theoretical dark matter that is a feature of several cosmological theories.

Neutron Star:

A neutron star is a type of remnant that can result from the gravitational collapse of a massive star during a Type II, Type Ib or Type Ic supernova event. Such stars are composed almost entirely of neutrons, which are subatomic particles with zero electrical charge and roughly the same mass as protons. Neutron stars are very hot and are supported against further collapse because of the Pauli exclusion principle. This principle requires that no two neutrons can occupy the same quantum state simultaneously.

Quark stars point to new matter


RX J1856.5-3754: Its size, just 11 km across, and temperature profile mean it cannot be a neutron star

Wednesday, 10 April, 2002

Astronomers believe they have found their first quark stars - super-dense objects that are formed when the remnants of old stars collapse in on themselves.Theorists have long suspected the existence of these weird objects, which are denser than neutron stars but are not compact enough to become black holes.The observations were made by the orbiting Chandra X-ray Observatory, and were unveiled at an American space agency (Nasa) press briefing in Washington, US.Quarks are incredibly tiny particles and make up much of the Universe. But on Earth, they are impossible to find on their own - they huddle together in groups of three, making up the protons and neutrons inside ordinary atoms.Knowledge of their existence is known from experiments in giant accelerator machines. Quarks are seen fleetingly in the debris from atoms that have been smashed together at very high speeds.

Strange threat:

But theory has long suggested that inside the superdense remains of dead stars, quarks might be forced out permanently into the open.They would make up a radically different state of matter called strange quark matter, so dense that a teaspoonful of it would weigh billions of tonnes.Now, astronomers say they have found two objects in space - one too small and one too cold - that defy "our understanding of the structure of matter". The Chandra researchers say these objects can only be understood if they consist of strange quark matter.Such quark stars are not dense enough to be black holes, but they are too dense to be anything else.The astronomers caution that further observations are needed to confirm their findings, but say that if they are right, quark stars will provide stunning insights into the nature of matter.Some scientists have suggested that if strange quark matter does exist, it could destroy ordinary matter by converting protons and neutrons to naked quarks, spreading through space like a cosmic wildfire.Now they know where to look, researchers will be able to judge what the chances are of this strange threat ever materialising.

Comet Threat More Constant Than Thought


Diagram showing the position of the Oort Cloud. Credit: Southwest Research Institute

11 December 2008

It certainly captures the imagination: a star passing silently by our solar system knocks a deadly barrage of comets towards Earth. However, recent simulations by one group of researchers has shown that these star-induced comet showers may not be as dramatic as once thought.The idea of nearby stars influencing comets goes back to 1950, when the astronomer Jan Hendrik Oort hypothesized an invisible repository of comets — the so-called Oort cloud — swarming around the solar system out to a distance of 100,000 AU (one AU is the distance between the sun and the Earth).
Oort assumed that stars passing through the cloud would cause a fresh batch of comets to fall in towards the sun, where they become visible to astronomers. Such a disturbance could have long-term effects."The comets we see now could be from a stellar passage hundreds of millions of years ago," said Hans Rickman of the Uppsala Astronomical Observatory in Sweden.However, Rickman and his colleagues have confirmed that star encounters alone cannot explain comet behavior. Using a computer model of the Oort cloud, they show that gravity effects from the galaxy are equally important. The results are reported in a recent article in the journal Celestial Mechanics and Dynamical Astronomy.

Two stars passing in the night

Although Earth has almost certainly been hit by comets throughout its history, it is not all that clear how often that has happened. Much of the crater history on Earth has been erased because of erosion or tectonic activity. The remaining craters could have come from asteroids instead of comets."It's quite difficult to tell a comet-induced crater from an asteroid one, since the impactor gets essentially vaporized," Rickman said.Comet impacts are, however, likely to be more energetic (and therefore more damaging), since comets are moving much faster than asteroids when they pass by Earth.Comet orbits can be altered whenever another star comes within 10,000 AU of our sun. Such a close encounter — occurring every 100 million years or so — will not typically disturb asteroids or planets, but it definitely "shakes up the whole Oort cloud," Rickman said.Most scientists have presumed that these star crossings will lead to a shower of comets raining down on the Earth and the rest of the inner solar system. Some have even claimed to find evidence of periodic mass extinctions that might be explained by a single (as-yet-unidentified) star in an elliptical orbit around the sun.To study the effect of stellar perturbations, Rickman and his colleagues model the Oort cloud with a sample of one million comets (the true number of cloud comets is unknown, but certainly much higher). The simulations are allowed to run for a time period corresponding to the 5-billion-year age of the solar system.The results show that stars can induce comet showers, but the contrast with non-shower periods is less than what people have thought before, Rickman said. This leveling out in comet activity is due to the influence of the gravitational field of the Milky Way.

Galactic tide

Astronomers have known for some time that our galaxy's gravity has an influence on the Oort cloud. Specifically, the cloud experiences a tidal effect due to the fact that the gravitational field is stronger the closer one is to the plane of the galaxy.The simulations by Rickman and colleagues show how the galactic tide constantly gives a small nudge to the cloud's comets. Some of these comets are in rather unstable orbits to begin with, so the slight push can send them on a sun-bound trajectory. Eventually, however, all these unstable comets are ejected from the solar system.And this is where stellar encounters become important. They scramble the Oort cloud, so that the galactic tide has a new crop of unstable comets to funnel into the inner solar system."The general picture spawned by our results is that injection of comets from the Oort Cloud is essentially to be seen as a teamwork involving both tides and stars," the scientists write in their paper.

This star-tide collaboration keeps a relatively steady supply of comets zooming nearby, so the threat from comet impacts probably does not change much over time.

Brown Dwarfs, Poorly Understood, Poorly Named


A cluster of nearly one thousand newly formed stars is captured in this infrared photograph as it emerges from the gaseous womb from which is was recently born. This extremely young cluster contains the largest known population of objects known as Brown Dwarfs. These are among the faintest sources present in the image.

07 June 2001

What's in a name? Sometimes, not much.

At a gathering in Germany this April of astronomers who study how planets and stars form, a poll was taken to determine whether brown dwarfs needed a new name.

The poll, however informal, represents the scientific community's acknowledgement that brown dwarfs exist in a gray area of definitions. They are cool, dim, but massive objects that so far do a lousy job of bridging our gap in understanding between planets and stars.

"Planetars" was suggested, as was "substellar objects" and host of other names.

Moderate debate ensued. No consensus was reached.

But with today's announcement that a significant number of brown dwarfs have protoplanetary disks around them, and hence must have formed just like stars do, the name "brown dwarf" now seems even less equipped to describe the objects.

Perhaps what brown dwarfs need is a real name, a single word, something memorable. Think planets, stars, comets, asteroids. Catchy names, all.

Charles J. Lada of the Smithsonian Astrophysical Observatory argues that "substellar objects" would now be the most apt moniker.

Prodded to consider that perhaps "substellar objects" wasn't exactly a catch term, Lada scratched his chin, tried to come up with something better, then decided that there was little chance the textbooks would be rewritten anyway.

Then he pointed out that this is all largely a semantic argument. Whatever we call brown dwarfs, they are still just stars that didn't make the grade.

And Nature, for its part, doesn't give a hoot.

"Nature doesn't see a difference between a brown dwarf and a star when it creates them," said August A. Muench of the University of Florida. The disk finding around brown dwarfs is the centerpiece of his doctoral dissertation.

But it sure makes enigmas out of the littler ones.

Earth Might Have Been a Ringed Planet, Like Saturn


Saturn, as seen by Cassini

17 September 2002

Earth may once have been surrounded by temporary rings of debris, much like Saturn, according to a new computer model that finds the rings might have cast parts of the planet into a twilight glow all day long.

The idea is not new, but the fresh modeling adds weight to the plausibility of an asteroid impact kicking up a sea of orbiting debris, and it considers how the rings would have cooled Earth's climate.

The new model, based on Saturns B-ring scaled down to Earth-size, was produced by Peter Fawcett of the University of New Mexico and Mark Boslough of the U.S. Department of Energys Sandia National Laboratories. It is based on climate models that had already been developed.

The scientists said a ring might form with a glancing blow, in which a space rock and the debris it carves from the planet ricochet into the atmosphere.

An expanding vapor cloud causes some of the debris to go into orbit. Over time, it collapses into a plane that matches Earth's equator. The ring then lasts from about 100,000 years to perhaps 1 million years at most.

Fawcett told the debris ring would have cooled the planet by blocking or reducing the amount of sunlight received in the tropics and subtropics. The rest of the planet would cool, too, because less heat would be transported from tropical regions to higher latitudes. That would mean fewer storms farther north.

The work is speculative, the researchers say, but there is some evidence they might be on the right track.

Geologic records reveal a layer of melted meteorite material thought to be associated with an asteroid impact 35.5 million years ago. Some 100,000 years of cooler global temperatures followed.

"This cooling is longer than one would expect from a large impact alone, so we hypothesized that a temporary ring might have formed," Fawcett said. "The jury is still out on this though."

Had there been any humans on the planet to survive the impact and witness the rings, it's hard to say exactly what they would have seen. But Boslough has some ideas, based on an assumption that the rings would have been semi-transparent, like Saturn's.

"For a person in the shadow of a reasonably opaque ring, it would be dark like twilight or a heavy overcast," he said. "The ring would be scattering light in addition to blocking it. I think the most spectacular view would be after sunset or before sunrise, when the sky is dark but parts of the sunlit ring would be brightly visible in the sky."

Habitable Planets: Four Types Proposed


The traditional view of our own solar system's habitable zone may be unfairly restrictive. This could also be the case for other systems. Credit: NASA

18 December 2008

The origin of life and the habitability of worlds other than Earth are two of the biggest mysteries facing science today. Much research has been dedicated to these topics, but there is still a lack of definite answers.

Jan Hendrik Bredehöft from the UK's Open University has been considering habitability on other worlds. "I'm one of those guys who takes a piece of meteorite, grinds it up and finds out what the organic chemistry is in there," said Bredehöft.

Based on these types of studies, he has come to believe that habitable worlds can be split into four categories, each with varying likelihoods of being home to extraterrestrial organisms. This has great potential for assisting the search for life in the universe, particularly as technology is now progressing to the stage where direct imaging of extrasolar planets is possible. Bredehöft presented his ideas at Europlanet's latest Planetary Science Congress.

His four groups of habitable worlds are: Earth-like, Mars-Like, Europa-like and water-worlds.

Taking each of these in turn, he considered their potential for hosting complex life. Earth-like words are the first class, and a kind of "control" since we already know such worlds are capable of sustaining complex life. Earth-like worlds feature an appropriate atmosphere, liquid water, moderate temperature ranges, and stable climates.

The second class of planets are those that were once much like Earth, such as Mars and Venus. "For some reason these planets left the classical habitable zone," said Bredehöft. "Mars became too dry, there's very little water left, at least not liquid water. Venus became just so enormously hot due to the greenhouse effect."

Still, Bredehöft believes there is some chance for life to exist on this type of world. He reasons that organisms could have developed when the planet was more hospitable, and this life could maintain a grip even through the hard times. "Once life has established itself it is really hard to kill off," said Bredehöft. "There have been absolutely devastating events in Earth's history that might have wiped out all kinds of life, but usually these served to further enhance biodiversity, rather than destroy it."

A chilly existence

Bodies that possess liquid water, but under an ice layer rather than on the surface, make up the third class of worlds.

Jupiter's moon Europa is a classic example from our own cosmic neighbourhood. Could there be life in places like this? Bredehöft's ideas here are particularly pertinent as often these worlds do not fit neatly into the conventional view of habitable zones. Europa, for example, lies beyond the solar system's temperature zone where water can remain as a liquid on a planet's surface.

However, there is still potential for life.

The traditional view of habitable zones thinks of a local star as being the prime energy source. But on icy worlds like Europa, other factors come into play, such as the gravitational pull of another planet. Worlds with liquid water hidden beneath icy layers could potentially be inhabited by simple organisms despite being far from the conventional habitable zone, so long as energy is provided in some other way.

Water-worlds

The fourth kind of habitable planets are made almost entirely of water. These hypothetical worlds would be Mercury to Earth-sized and would feature extensive oceans. Unlike oceans on Earth, the water on these types of planets would not be in contact with silicates or other rocks.

"These planets can either be completely made of water with high pressure ice at the core, or they can have bodies of liquid water that are separated from a silicate core by a thick layer of high pressure ice," said Bredehöft.

One theory for life's origin on Earth says organic material collected in shallow pools and then became concentrated by clinging to the surface of rocks. Eventually, this early life spread into the wider ocean. Another theory for life's origin is that the necessary chemistry occurred at hydrothermal volcanic vents. On water worlds, however, these scenarios are impossible. Therefore, Bredehöft thinks life is not likely to originate on such planets.

"The amount of water on such a planet would be so huge, you would need unbelievable amounts of carbon components concentrated together for a chance of life. It's far too diluted," said Bredehöft.

Considered opinions

After considering all the facts, Bredehöft said the best bet to find extraterrestrial ecosystems is to hunt for Earth-like planets, after all. However, he doesn't think Earth-like worlds will necessarily have advanced life.

"We don't know whether the level of complexity or the size of organisms living on Earth is essentially a logical outcome of evolution or whether it is just some fluke experienced here," said Bredehöft. "Is having talking intelligent beings on the surface of the planet the pinnacle of evolution? We just assume so because we like to see ourselves as something special."

With the rapid pace of development in planet-hunting technology, it is only a matter of time until we learn much more about exotic extrasolar planets and moons, and are able to glean vital information about their properties. Until then though, scientists like Bredehöft will continue to theorise about discoveries.

So in Bredehöft's carefully considered opinion, what kind of organisms are we most likely to find? "Probably something slimy," he said.

Saturday, December 27, 2008

Ergosphere



The two surfaces on which the Kerr metric appears to have singularities; the inner surface is the spherical event horizon, whereas the outer surface is an oblate spheroid. The ergosphere lies between these two surfaces; within this volume, the purely temporal component gtt is negative, i.e., acts like a purely spatial metric component. Consequently, particles within this ergosphere must co-rotate with the inner mass, if they are to retain their time-like character.

The ergosphere is a region located outside a rotating black hole. Its name is derived from the Greek word ergon, which means “work”. It received this name because it is theoretically possible to extract energy and mass from the black hole in this region.The ergosphere is ellipsoidal in shape and is situated so that at the poles of rotating black hole it touches the event horizon and stretches out to a distance that is equal to the radius of the event horizon. Within the ergosphere spacetime is dragged along in the direction of the rotation of the black hole at a speed greater than the speed of light in relation to the rest of the universe. This process is known as the Lense-Thirring effect or frame-dragging. Because of this dragging effect objects within the ergosphere are not stationary with respect to the rest of the universe, unless they travel faster than the speed of light, which is impossible based on the laws of physics. Another result of this dragging of space is the existence of negative energies within the ergosphere.

The outer limit of the ergosphere is the stationary limit. At the stationary limit objects moving at the speed of light are stationary with respect to the rest of the universe. This is because the space here is being dragged at exactly the speed of light relative to the rest of space. Outside this limit space is still dragged, but at a rate less than the speed of light.

Since the ergosphere is outside the event horizon, it is still possible for objects to escape from the gravitational pull of the black hole. An object can gain energy by entering the black hole’s rotation and then escaping from it, thus taking some of the black hole's energy with it. This process of removing energy from a rotating black hole was proposed by the mathematician Roger Penrose in 1969, and is called the Penrose process. The theoretical maximum of possible energy extraction is 29% of the total energy of a rotating black hole. Once this energy is removed the black hole loses its spin and the ergosphere no longer exists. This process is considered a possible explanation for a source of energy of such energetic phenomena as gamma ray bursts. Results from computer models show that the Penrose Process is capable of producing the high energy particles that are observed being emitted from quasars and other active galactic nuclei.

Biggest black hole in the Universe discovered


An artist's conception of a supermassive black hole accreting from a disk. Credit: NASA/JPL-Caltech

The most massive known black hole in the universe has been discovered, weighing in with the mass of 18 billion Suns. Observing the orbit of a smaller black hole around this monster has allowed astronomers to test Einstein's theory of general relativity with stronger gravitational fields than ever before.The black hole is about six times as massive as the previous record holder and in fact weighs as much as a small galaxy. It lurks 3.5 billion light years away, and forms the heart of a quasar called OJ287. A quasar is an extremely bright object in which matter spiralling into a giant black hole emits copious amounts of radiation.But rather than hosting just a single colossal black hole, the quasar appears to harbour two - a setup that has allowed astronomers to accurately 'weigh' the larger one.The smaller black hole, which weighs about 100 million Suns, orbits the larger one on an oval-shaped path every 12 years. It comes close enough to punch through the disc of matter surrounding the larger black hole twice each orbit, causing a pair of outbursts that make OJ287 suddenly brighten.General relativity predicts that the smaller hole's orbit itself should rotate, or precess, over time, so that the point at which it comes nearest its neighbour moves around in space - an effect seen in Mercury's orbit around the Sun, albeit on a smaller scale.

Bright outbursts:

In the case of OJ287, the tremendous gravitational field of the larger black hole causes the smaller black hole's orbit to precess at an incredible 39° each orbit. The precession changes where and when the smaller hole crashes through the disc surrounding its larger sibling.About a dozen of the resulting bright outbursts have been observed to date, and astronomers led by Mauri Valtonen of Tuorla Observatory in Finland have analysed them to measure the precession rate of the smaller hole's orbit. That, along with the period of the orbit, suggests the larger black hole weighs a record 18 billion Suns.A couple of other black holes have been estimated to be as massive, but their masses are less certain, says Valtonen. That's because the estimates were based on the speed of gas clouds around the black holes, and it is not clear whether the clouds are simply passing by the black holes or actually orbiting them.But Tod Strohmayer of NASA's Goddard Space Flight Center in Maryland, US, says he is not convinced that Valtonen's team has really measured the mass of the large black hole in OJ287 accurately.That's because only a handful of the outbursts have been measured with high precision, making it difficult to determine if the precession scenario is responsible for the outbursts. "Obviously, if subsequent timings continue to agree with the model, then that would provide further support," he told.

No limit:

Just how big can black holes get? Craig Wheeler of the University of Texas in Austin, US, says it depends only on how long a black hole has been around and how fast it has swallowed matter in order to grow. "There is no theoretical upper limit," he says.The new research also tested another prediction of general relativity - that the black holes should spiral towards each other as they radiate energy away in the form of gravitational waves, or ripples in space. This radiation affects the timing of the disc crossings and their accompanying outbursts.The most recent outburst occurred on 13 September 2007, as predicted by general relativity. "If there was no orbital decay, the outburst would have been 20 days later than when it actually happened," Valtonen told, adding that the black holes are on track to merge within 10,000 years.Wheeler says the observations of the outbursts fit closely with the expectations from general relativity. "The fact that you can fit Einstein's theory [so well] ... is telling you that that's working," he says.

The research was presented on Wednesday at a meeting of the American Astronomical Society in Austin, Texas, US.

Techniques for finding black holes


Formation of extragalactic jets from a black hole's accretion disk

Accretion disks and gas jets:

Most accretion disks and gas jets are not clear proof that a stellar-mass black hole is present, because other massive, ultra-dense objects such as neutron stars and white dwarfs cause accretion disks and gas jets to form and to behave in the same ways as those around black holes. But they can often help by telling astronomers where it might be worth looking for a black hole.On the other hand, extremely large accretion disks and gas jets may be good evidence for the presence of supermassive black holes, because as far as we know any mass large enough to power these phenomena must be a black hole.

Strong radiation emissions:

Steady X-ray and gamma ray emissions also do not prove that a black hole is present, but can tell astronomers where it might be worth looking for one - and they have the advantage that they pass fairly easily through nebulae and gas clouds.But strong, irregular emissions of X-rays, gamma rays and other electromagnetic radiation can help to prove that a massive, ultra-dense object is not a black hole, so that "black hole hunters" can move on to some other object. Neutron stars and other very dense stars have surfaces, and matter colliding with the surface at a high percentage of the speed of light will produce intense flares of radiation at irregular intervals. Black holes have no material surface, so the absence of irregular flares around a massive, ultra-dense object suggests that there is a good chance of finding a black hole there.Intense but one-time gamma ray bursts (GRBs) may signal the birth of "new" black holes, because astrophysicists think that GRBs are caused either by the gravitational collapse of giant stars or by collisions between neutron stars, and both types of event involve sufficient mass and pressure to produce black holes. But it appears that a collision between a neutron star and a black hole can also cause a GRB,so a GRB is not proof that a "new" black hole has been formed. All known GRBs come from outside our own galaxy, and most come from billions of light years away so the black holes associated with them are actually billions of years old.Some astrophysicists believe that some ultraluminous X-ray sources may be the accretion disks of intermediate-mass black holes.Quasars are thought to be the accretion disks of supermassive black holes, since no other known object is powerful enough to produce such strong emissions. Quasars produce strong emission across the electromagnetic spectrum, including UV, X-rays and gamma-rays and are visible at tremendous distances due to their high luminosity. Between 5 and 25% of quasars are "radio loud," so called because of their powerful radio emission.

Gravitational lensing:

A gravitational lens is formed when the light from a very distant, bright source (such as a quasar) is "bent" around a massive object (such as a black hole) between the source object and the observer. The process is known as gravitational lensing, and is one of the predictions of the general theory of relativity. According to this theory, mass "warps" space-time to create gravitational fields and therefore bend light as a result.A source image behind the lens may appear as multiple images to the observer.
Black hole detect
Lensing by a black hole. Animated simulation of gravitational lensing caused by a going past a background galaxy. A secondary image of the galaxy can be seen within the black hole Einstein ring on the opposite direction of that of the galaxy. The secondary image grows (remaining within the Einstein ring) as the primary image approaches the black hole. The surface brightness of the two images remain constant, but their angular size vary, hence producing an amplification of the galaxy luminosity as seen from a distant observer. The maximum amplification occurs when the background galaxy (or in the present case a bright part of it) is exactly behind the black hole.

In cases where the source, massive lensing object, and the observer lie in a straight line, the source will appear as a ring behind the massive object.
Gravitational lensing can be caused by objects other than black holes, because any very strong gravitational field will bend light rays. Some of these multiple-image effects are probably produced by distant galaxies.

Determining the mass of black holes:

Quasi-periodic oscillations can be used to determine the mass of black holes.The technique uses a relationship between black holes and the inner part of their surrounding disks, where gas spirals inward before reaching the event horizon. As the gas collapses inwards, it radiates X-rays with an intensity that varies in a pattern that repeats itself over a nearly regular interval. This signal is the Quasi-Periodic Oscillation, or QPO. A QPO’s frequency depends on the black hole’s mass; the event horizon lies close in for small black holes, so the QPO has a higher frequency. For black holes with a larger mass, the event horizon is farther out, so the QPO frequency is lower.

Objects orbiting possible black holes:

Objects orbiting black holes probe the gravitational field around the central object. An early example, discovered in the 1970s, is the accretion disk orbiting the putative black hole responsible for Cygnus X-1, a famous X-ray source. While the material itself cannot be seen directly, the X rays flicker on a millisecond time scale, as expected for hot clumpy material orbiting a ~10 solar-mass black hole just prior to accretion.

A Chandra X-ray spectrum of Cygnus X-1 showing a characteristic peak near 6.4 keV due to ionized iron in the accretion disk, but the peak is gravitationally red-shifted, broadened by the Doppler effect, and skewed toward lower energies

The X-ray spectrum exhibits the characteristic shape expected for a disk of orbiting relativistic material, with an iron line, emitted at ~6.4 keV, broadened to the red (on the receding side of the disk) and to the blue (on the approaching side).Another example is the star S2, seen orbiting the Galactic center. Here the star is several light hours from the ~3.5×106 solar mass black hole, so its orbital motion can be plotted. Nothing is observed at the center of the observed orbit, the position of the black hole itself——as expected for a black object.