Stars Falling From The Sky Episode 19, You are watching Stars Falling From the Sky Episode 19 from the Stars Falling From the Sky Series. Watch Stars Falling From the Sky Episode 19 and the other episodes of Stars Falling From the Sky with english subs only here at ep drama.

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Fairy Tail episode 22 | Watch Fairy Tail 22 English Sub Online episode.  Yeah the thrilling and exciting adventure from Fairy Tail episode 22 is coming. Fans will ask that question that where can i watch this video. The answer is simple that you can watch Fairy Tail episode 22 Online after its release. Fairy Tail videos are broadcast on popular TV channels and local networks. You can just go there and watch this newly available videos.

Fairy Tail episode 22 is releasing with the title with “Episode 22″. Enjoy every minute of this 25 minutes video and don’t forget to watch this video on Monday 15 March 2010, So never forget to comeback here and see the latest updates.

Texas Alabama Score updates :- Alabama withstood a late rally by Texas, but forced a late turnover and Mark Ingram’s second touchdown of the night finished off Texas’ run and secured the Crimson Tide’s 13th National Championship with a 37-21 win.

Mark Ingram, the Heisman trophy winner, was awarded the game’s Offensive MVP award. Defensive MVP honors went to Marcell Dareus who knocked Colt McCoy out of the game and returned an interception for a touchdown.

Texas Stars (21-11-2-4, 48 points) defeated the Houston Aeros (18-15-5-1, 42 points) 3-2 in overtime on Tuesday night in front of 4,927 fans at Cedar Park Center. Texas defenseman Ivan Vishnevskiy scored with 38 seconds left in overtime to lift the Stars over the Aeros. Stars forward Warren Peters started a three-goal Texas rally with a power-play goal in the first period. He also added an assist on the game-winning goal as the Stars ended a five-game winless skid (0-3-0-2). Texas Stars goalie Matt Climie (10-10-3) stopped 19 Houston shots in the team’s 10th home win of the year. Texas forward Mathieu Beaudoin also scored in the victory, the Stars first win at home since Dec. 11. Aeros goalie Anton Khudobin (9-11-2) made 21 saves in the overtime loss. Texas will play in Abbotsford, BC at 9:30 pm (CST)

Golden Disk Awards 2009, It’s December 10th, 2009 and the 24th Golden Disk Awards are finally here! Before the actual ceremony got underway, there was the customary red carpet where our favourite stars walked the runway. Check out the photos of the stars that gathered under the night skies!

Fiona Xie Boyfriend, Fiona Xie,The 27-year-old actress explained in an interview published on this weeks’s 8 Days magazine that she did not set out to avoid the media but was simply weary of the complications speaking to them would bring.

As for the “personal reasons” for rejecting the role, Xie said she could not find her character’s voice though she admits that she gave it up partly because of her Australian-American boyfriend.

According to the actress, her boyfriend did not like the script as it contained too many kissing scenes, so she turned it down.

“He wanted me to ask for amendments to the script so I have less kissing scenes. I know that is impossible but I don’t want him to be unhappy,” she explained.

Xie’s 23-year-old squeeze is an enigma. They first met on the set of Kelvin Tong’s supernatural thriller “Rule #1″ in 2007 and have been dating for a year, and he is reportedly an art enthusiast who lives like royalty in Hong Kong, but everything else about him remains a mystery.

The actress who has been dubbed one of MediaCorp’s Seven Princesses, was named Best Newcomer in her first year and was twice voted one of the top ten most popular actresses by viewers at the annual Star Awards.

Her decision to drop everything and base herself Hong Kong will force her to bid goodbye to her annual salary of about S$500,000. However, it will afford her greater control over her life and gives her the freedom to choose what projects she wants to do.

She said that while she is concerned that this loss of income might affect the livelihood of her mother and her younger brother, Dylan, who is sill studying, she is determined to get a fresh start in Hong Kong. The actress, who had recently embraced Christianity, has no regrets.

Dancing With The Stars Vote Online, The remaining three celebrities and their professional dance partners will face one last time. Mya and Dmitry Chaplin will deliver the best results, but Kelly Osbourne and Louis Van Amstel, and Donny Osmond and Kym Johnson has a fan base and can become successful too.

Each pair will make three balls. Each performs a ballroom or Latin dance, a dance freestyle megamix and challenge. Mya and Chaplin performing a paso doble, which they did as part of the double team step in the 7th week of competition to Joan Jett “I Hate Myself For Loving You” is a score of 24. Osbourne and Van Amstel and Osmond and Johnson competed on the winning team of Tango.

Kelly Osbourne and Louis Van Amstel danced the Argentine tango. Mya and Chaplin and Osmond and Johnson performed the Argentine tango during week five with Osmond and Johnson get a 29 and Mya and Chaplin win by 27.

Donny Osmond and Kym Johnson will face the cha cha cha. Mya and Chaplin won by 29 last week with their cha cha cha and Osbourne and Van Amstel got a 27 (also last week).

The megamix is a group dance number, where the three couples will perform at the same time and by the mixture is that the styles of dance will be the Viennese waltz, samba and jive.

News and views updates about Dancing with the stars Michael Jackson tribute, If you missed it, check out the Dancing with the Stars Michael Jackson tribute performance from the October 20 results show in this DWTS video clip.

DWTS host Tom Bergeon explained that organizing the tribute was a natural choice, in light of the fact that contestants had already performed to Michael Jackson’s hits 17 times during the show’s four-year run.

NASA’s first mission capable of finding Earth-size and smaller planets around other stars.

Importance of Planet Detection

The centuries-old quest for other worlds like our Earth has been rejuvenated by the intense excitement and popular interest surrounding the discovery of hundreds of planets orbiting other stars.

There is now clear evidence for substantial numbers of three types of exoplanets; gas giants, hot-super-Earths in short period orbits, and ice giants. The following websites are tracking the day-by-day increase in new discoveries and are providing information on the characteristics of the planets as well as those of the stars they orbit: Extrasolar Planets Encyclopedia, New Worlds Atlas, and Current Planet Count Widget.

The challenge now is to find terrestrial planets (i.e., those one half to twice the size of the Earth), especially those in the habitable zone of their stars where liquid water and possibly life might exist.

The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets.

Results from this mission will allow us to place our solar system within the continuum of planetary systems in the Galaxy.

Page Contents:

* Introduction
* Science Objectives
* The Transit Method of Detecting Extrasolar Planets
* Mission design
* Expected Results
* Flight System Characteristics
* Mission Characteristics

The Extended Solar Neighborhood

The figure shows what we believe to be the local structure of our Galaxy, the Milky Way. The stars sampled are similar to the immediate solar neighborhood. Young stellar clusters, ionized hydrogen (HII) regions and the neutral hydrogen (HI) distribution define the arms of the Galaxy.

To Page Contents
Kepler Mission Scientific Objective:

The scientific objective of the Kepler Mission is to explore the structure and diversity of planetary systems. This is achieved by surveying a large sample of stars to:

1. Determine the percentage of terrestrial and larger planets there are in or near the habitable zone of a wide variety of stars;
2. Determine the distribution of sizes and shapes of the orbits of these planets;
3. Estimate how many planets there are in multiple-star systems;
4. Determine the variety of orbit sizes and planet reflectivities, sizes, masses and densities of short-period giant planets;
5. Identify additional members of each discovered planetary system using other techniques; and
6. Determine the properties of those stars that harbor planetary systems.

The Kepler Mission also supports the objectives of future NASA Origins theme missions Space Interferometry Mission (SIM) and Terrestrial Planet Finder (TPF),

* By identifying the common stellar characteristics of host stars for future planet searches,
* By defining the volume of space needed for the search and
* By allowing SIM to target systems already known to have terrestrial planets.

To Page Contents
The Transit Method of Detecting Extrasolar Planets:

When a planet crosses in front of its star as viewed by an observer, the event is called a transit. Transits by terrestrial planets produce a small change in a star’s brightness of about 1/10,000 (100 parts per million, ppm), lasting for 2 to 16 hours. This change must be absolutely periodic if it is caused by a planet. In addition, all transits produced by the same planet must be of the same change in brightness and last the same amount of time, thus providing a highly repeatable signal and robust detection method.

Once detected, the planet’s orbital size can be calculated from the period (how long it takes the planet to orbit once around the star) and the mass of the star using Kepler’s Third Law of planetary motion. The size of the planet is found from the depth of the transit (how much the brightness of the star drops) and the size of the star. From the orbital size and the temperature of the star, the planet’s characteristic temperature can be calculated. From this the question of whether or not the planet is habitable (not necessarily inhabited) can be answered.

To Page Contents
The Kepler Mission Design

For a planet to transit, as seen from our solar system, the orbit must be lined up edgewise to us. The probability for an orbit to be properly aligned is equal to the diameter of the star divided by the diameter of the orbit. This is 0.5% for a planet in an Earth-like orbit about a solar-like star. (For the giant planets discovered in four-day orbits, the alignment probability is more like 10%.) In order to detect many planets one can not just look at a few stars for transits or even a few hundred. One must look at thousands of stars, even if Earth-like planets are common. If they are rare, then one needs to look at many thousands to find even a few. Kepler looks at 100,000 stars so that if Earths are rare, a null or near null result would still be significant. If Earth-size planets are common then Kepler should detect hundreds of them.

Considering that we want to find planets in the habitable zone, the time between transits is about one year. To reliably detect a sequence one needs four transits. Hence, the mission duration needs to be at least three and one half years.

The Kepler instrument is a specially designed 0.95-meter diameter telescope called a photometer or light meter. It has a very large field of view for an astronomical telescope — 105 square degrees, which is comparable to the area of your hand held at arm’s length. The fields of view of most telescopes are less than one square degree. Kepler needs that large a field—105 square degrees—in order to observe the necessary large number of stars. It stares at the same star field for the entire mission and continuously and simultaneously monitors the brightnesses of more than 100,000 stars for the life of the mission—3.5 years.

The diameter of the telescope needs to be large enough to reduce the noise from photon counting statistics, so that it can measure the small change in brightness of an Earth-like transit. The design of the entire system is such that the combined differential photometric precision over a 6.5 hour integration is less than 20 ppm (one-sigma) for a 12th magnitude solar-like star including an assumed stellar variability of 10 ppm. This is a conservative, worse-case assumption of a grazing transit. A central transit of the Earth crossing the Sun lasts 13 hours. And about 75% of the stars older than 1 Gyr are less variable then the Sun on the time scale of a transit.

The photometer must be spacebased to obtain the photometric precision needed to reliably see an Earth-like transit and to avoid interruptions caused by day-night cycles, seasonal cycles and atmospheric perturbations, such as, extinction associated with ground-based observing.

Extending the mission beyond three and one half years provides for:

1. Improving the signal to noise by combining more transits to permit detection of smaller planets
2. Finding planets in orbits with larger periods
3. Finding planets around stars that are noisier either due to being fainter or having more variability

Expected Results:

Based on the mission described above, including conservative assumptions about detection criteria, stellar variability, taking into account only orbits with 4 transits in 3.5 years, etc., and assuming that planets are common around other stars like our Sun, then we expect to detect:

From transits of terrestrial planets in one year orbits:

* About 50 planets if most are the same size as Earth (R~1.0 Re) and none larger,
* About 185 planets if most have a size of R~1.3 Re,
* About 640 planets if most have a size of R~2.2 Re,
* About 12% with two or more planets per system.

These numbers come out substantially higher, when one takes into consideration all orbits from a few days to more than one year.

From modulation of the reflected light from giant inner planets:

* About 870 planets with periods less than one week.

From transits of giant planets:

* About 135 inner-orbit planet detections,
* Densities for 35 inner-orbit planets, and
* About 30 outer-orbit planet detections.

Detection of the short-period giant planets should occur within the first several months of the mission.

The sample size of stars for this mission is large enough to capture the richness of the unexpected. Should no detection be made, a null result would still be very significant.

To Page Contents
System Characteristics:

Spacebased Photometer: 0.95-m aperture

Primary mirror: 1.4 meter diameter, 85% light weighted

Detectors: 95 mega pixels (42 CCDs with 2200

NASA’s first mission capable of finding Earth-size and smaller planets around other stars.

Importance of Planet Detection

The centuries-old quest for other worlds like our Earth has been rejuvenated by the intense excitement and popular interest surrounding the discovery of hundreds of planets orbiting other stars.

There is now clear evidence for substantial numbers of three types of exoplanets; gas giants, hot-super-Earths in short period orbits, and ice giants. The following websites are tracking the day-by-day increase in new discoveries and are providing information on the characteristics of the planets as well as those of the stars they orbit: Extrasolar Planets Encyclopedia, New Worlds Atlas, and Current Planet Count Widget.

The challenge now is to find terrestrial planets (i.e., those one half to twice the size of the Earth), especially those in the habitable zone of their stars where liquid water and possibly life might exist.

The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets.

Results from this mission will allow us to place our solar system within the continuum of planetary systems in the Galaxy.

Page Contents:

* Introduction
* Science Objectives
* The Transit Method of Detecting Extrasolar Planets
* Mission design
* Expected Results
* Flight System Characteristics
* Mission Characteristics

The Extended Solar Neighborhood

The figure shows what we believe to be the local structure of our Galaxy, the Milky Way. The stars sampled are similar to the immediate solar neighborhood. Young stellar clusters, ionized hydrogen (HII) regions and the neutral hydrogen (HI) distribution define the arms of the Galaxy.

To Page Contents
Kepler Mission Scientific Objective:

The scientific objective of the Kepler Mission is to explore the structure and diversity of planetary systems. This is achieved by surveying a large sample of stars to:

1. Determine the percentage of terrestrial and larger planets there are in or near the habitable zone of a wide variety of stars;
2. Determine the distribution of sizes and shapes of the orbits of these planets;
3. Estimate how many planets there are in multiple-star systems;
4. Determine the variety of orbit sizes and planet reflectivities, sizes, masses and densities of short-period giant planets;
5. Identify additional members of each discovered planetary system using other techniques; and
6. Determine the properties of those stars that harbor planetary systems.

The Kepler Mission also supports the objectives of future NASA Origins theme missions Space Interferometry Mission (SIM) and Terrestrial Planet Finder (TPF),

* By identifying the common stellar characteristics of host stars for future planet searches,
* By defining the volume of space needed for the search and
* By allowing SIM to target systems already known to have terrestrial planets.

To Page Contents
The Transit Method of Detecting Extrasolar Planets:

When a planet crosses in front of its star as viewed by an observer, the event is called a transit. Transits by terrestrial planets produce a small change in a star’s brightness of about 1/10,000 (100 parts per million, ppm), lasting for 2 to 16 hours. This change must be absolutely periodic if it is caused by a planet. In addition, all transits produced by the same planet must be of the same change in brightness and last the same amount of time, thus providing a highly repeatable signal and robust detection method.

Once detected, the planet’s orbital size can be calculated from the period (how long it takes the planet to orbit once around the star) and the mass of the star using Kepler’s Third Law of planetary motion. The size of the planet is found from the depth of the transit (how much the brightness of the star drops) and the size of the star. From the orbital size and the temperature of the star, the planet’s characteristic temperature can be calculated. From this the question of whether or not the planet is habitable (not necessarily inhabited) can be answered.

To Page Contents
The Kepler Mission Design

For a planet to transit, as seen from our solar system, the orbit must be lined up edgewise to us. The probability for an orbit to be properly aligned is equal to the diameter of the star divided by the diameter of the orbit. This is 0.5% for a planet in an Earth-like orbit about a solar-like star. (For the giant planets discovered in four-day orbits, the alignment probability is more like 10%.) In order to detect many planets one can not just look at a few stars for transits or even a few hundred. One must look at thousands of stars, even if Earth-like planets are common. If they are rare, then one needs to look at many thousands to find even a few. Kepler looks at 100,000 stars so that if Earths are rare, a null or near null result would still be significant. If Earth-size planets are common then Kepler should detect hundreds of them.

Considering that we want to find planets in the habitable zone, the time between transits is about one year. To reliably detect a sequence one needs four transits. Hence, the mission duration needs to be at least three and one half years.

The Kepler instrument is a specially designed 0.95-meter diameter telescope called a photometer or light meter. It has a very large field of view for an astronomical telescope — 105 square degrees, which is comparable to the area of your hand held at arm’s length. The fields of view of most telescopes are less than one square degree. Kepler needs that large a field—105 square degrees—in order to observe the necessary large number of stars. It stares at the same star field for the entire mission and continuously and simultaneously monitors the brightnesses of more than 100,000 stars for the life of the mission—3.5 years.

The diameter of the telescope needs to be large enough to reduce the noise from photon counting statistics, so that it can measure the small change in brightness of an Earth-like transit. The design of the entire system is such that the combined differential photometric precision over a 6.5 hour integration is less than 20 ppm (one-sigma) for a 12th magnitude solar-like star including an assumed stellar variability of 10 ppm. This is a conservative, worse-case assumption of a grazing transit. A central transit of the Earth crossing the Sun lasts 13 hours. And about 75% of the stars older than 1 Gyr are less variable then the Sun on the time scale of a transit.

The photometer must be spacebased to obtain the photometric precision needed to reliably see an Earth-like transit and to avoid interruptions caused by day-night cycles, seasonal cycles and atmospheric perturbations, such as, extinction associated with ground-based observing.

Extending the mission beyond three and one half years provides for:

1. Improving the signal to noise by combining more transits to permit detection of smaller planets
2. Finding planets in orbits with larger periods
3. Finding planets around stars that are noisier either due to being fainter or having more variability

Expected Results:

Based on the mission described above, including conservative assumptions about detection criteria, stellar variability, taking into account only orbits with 4 transits in 3.5 years, etc., and assuming that planets are common around other stars like our Sun, then we expect to detect:

From transits of terrestrial planets in one year orbits:

* About 50 planets if most are the same size as Earth (R~1.0 Re) and none larger,
* About 185 planets if most have a size of R~1.3 Re,
* About 640 planets if most have a size of R~2.2 Re,
* About 12% with two or more planets per system.

These numbers come out substantially higher, when one takes into consideration all orbits from a few days to more than one year.

From modulation of the reflected light from giant inner planets:

* About 870 planets with periods less than one week.

From transits of giant planets:

* About 135 inner-orbit planet detections,
* Densities for 35 inner-orbit planets, and
* About 30 outer-orbit planet detections.

Detection of the short-period giant planets should occur within the first several months of the mission.

The sample size of stars for this mission is large enough to capture the richness of the unexpected. Should no detection be made, a null result would still be very significant.

To Page Contents
System Characteristics:

Spacebased Photometer: 0.95-m aperture

Primary mirror: 1.4 meter diameter, 85% light weighted

Detectors: 95 mega pixels (42 CCDs with 2200

Kepler Mission, A team of scientists has solved a longstanding mystery about a pair of stars called DI Herculis whose peculiar rotation had remained a mystery for three decades.

The shift in the orbit of DI Herculis was a mystery till now.

Now, MIT (Massachusetts Institute Of Technology) researchers and colleagues have determined that the stars are rotating tipped over on their sides, relative to their orbits around each other.

This produces tidal effects that counteract the expected rate for the orbits to shift orientation over time (called precession), finally explaining the mysterious anomaly.

The discrepancy in the rate of precession had been seen as a possible refutation of Einstein’s theory of relativity, so finding a conventional explanation means that relativity has withstood another possible challenge.

This discovery could also help to shed light on how binary stars (about half of all known stars) are formed and how their rotation and orbits evolve over time.

The mystery was solved by postdoctoral researcher Simon Albrecht and assistant professor of physics Joshua Winn and others, who used a high-resolution spectrograph called Sophie on a 1.93-meter telescope at the Observatoire de Haute-Provence in France to make highly detailed observations that revealed the unexpected tilt – one of more than 70 degrees from vertical, the other more than 80 degrees – of the stars’ rotation axes.

The team now hopes to study other unusual binary stars to try to determine how unusual this tipped-over configuration is.