Orion Nebula, 1881 Vs. 2011 Via Imgur

He had a long, fair-skinned face with a very thoughtful expression. This was partially concealed by surprisingly long, blond hair, most of which was tied behind his head, but he also had very long bangs, which he was probably always pushing out of his eyes, and a long lock of hair hanging down in front of each ear. The eyes were a startling green, a shade not normally achieved on Earth without the assistance of contact lenses.

Postcards from Mars

yall arent ready yet but one day were going to talk about how the young wizards series is better than harry potter. the language is more complicated but trust me, its better 

Y’all I’m positively howling, it’s almost EXACTLY what Dairine said to Nita about Kit waaay back in Deep Wizardry

Paging the newly-fledged-and-recruiting Dairine/Mehrnaz squad @hencegoodfortune @shamrockjolnes @inkidink @imaginariumgeographica

Vera Rubin (b. 1928)

When Vera Cooper Rubin told her high school physics teacher that she’d been accepted to Vassar, he said, “That’s great. As long as you stay away from science, it should be okay.”

Rubin graduated Phi Beta Kappa in 1948, the only astronomy major in her class at Vassar, and went on to receive her master’s from Cornell in 1950 (after being turned away by Princeton because they did not allow women in their astronomy program) and her Ph.D. from Georgetown in 1954. Now a senior researcher at the Carnegie Institute’s Department of Terrestrial Magnetism, Rubin is credited with proving the existence of “dark matter,” or nonluminous mass, and forever altering our notions of the universe. She did so by gathering irrefutable evidence to persuade the astronomical community that galaxies spin at a faster speed than Newton’s Universal Law of Gravitation allows. As a result of this finding, astronomers conceded that the universe must be filled with more material than they can see. 

Rubin made a name for herself not only as an astronomer but also as a woman pioneer; she fought through severe criticisms of her work to eventually be elected to the National Academy of Sciences (at the time, only three women astronomers were members) and to win the highest American award in science, the National Medal of Science. Her master’s thesis, presented to a 1950 meeting of the American Astronomical Society, met with severe criticism, and her doctoral thesis was essentially ignored, though her conclusions were later validated. “Fame is fleeting,” Rubin said when she was elected to the National Academy of Sciences. “My numbers mean more to me than my name. If astronomers are still using my data years from now, that’s my greatest compliment.”

 Sources:

1. http://innovators.vassar.edu/innovator.html?id=68; http://science.vassar.edu/women/

2. http://dspace.mit.edu/handle/1721.1/45424

The galaxy sings in B flat. Fifty-seven octaves below middle C, hundreds of thousands of tiny stars with little worlds trailing atmospheres in elliptical orbits. Double-star systems, triple-star, more; planets, civilisations, dark matter, tangible matter, all circling, swarming, humming together in one enormous note, not bumping together but carrying a wave from the centre of their island universe, expanding out into space… Sound cannot exist in a vacuum. This is a widely known fact. And space is a vacuum, sure. But only when you look at it from here, from our tiny little world. Close your eyes, zoom out, and look at the celestial spheres from their view; and space isn’t so thin after all. Close your eyes, zoom in, and even our dense atmosphere is just atoms in a vacuum of their own. Sound as we know it, sure, that doesn’t exist outside our little stardust orb. It’s too small, too fragile. Too like ourselves. But where there’s movement and things to move, there’s sound. Sound waves can be small, only a few thousand nanometres trough-to-crest. And they can be massive, playing the celestial music of the spheres. Because in all that movement, the pulses of our discs and and lights and gravity wells, the stars dance. We are sound, the particles that carry a wave thousands of light-years across. We are the music of the celestial spheres. The galaxy sings in B flat.

Source

anexpansionlikegold

NATASHA I DEMAND YOU HAVE THESE FEELS WITH ME

(via reconfemmandoforares)

Fridge thought fully like, twenty years later, when thinking about the concept in Young Wizards about how a wizard is picked to be offered wizardry and given an Ordeal because they're exactly the right person for a particular problem:

So Dairine, given the power of wizardry, decides to go find Darth Vader and kick his ass, right?

And there’s like some discussion about how, if she uses her raw wizardly power to ‘go find Darth Vader’ then she’s inevitably going to end up attracting the attention of the universe’s equivalent thereof.

Which okay I always just nodded along to the logic of, big bad guy=big bad guy.

But what my brain somehow failed to conceptualize, and this may have been obvious to some other people, is what happens to Darth Vader at the end of the movies

Namely. He gets redeemed, because someone is willing to reach out and help him along towards that.

She didn’t just summon the attention of the Lone Power by trying to manifest Darth Vader into the universe by sheer ten year old stubborness, she summoned SPECIFICALLY the version of the Lone Power where Reconfiguration was a built-in possibility.

Kepler Mission Analysis Shows Reduced Number of Earth-Sized Planets in Field of View

A large number of worlds found by NASA’s Kepler alien planet-hunting space telescope are probably significantly larger than scientists previously estimated, a new study suggests. Using a galaxy similar to our own Milky Way, the image above shows the scale of the distances for the sample of stars with planet candidates described in a new study by scientists using the Kitt Peak National Observatory Mayall 4-meter telescope . The circled dot represents the position of the sun in the Milky Way, and the stippled cone shows how far away the new candidate stars are (2800-7000 light years), compared to the size of our galaxy. 

The Kepler Space Telescope has spotted more than 2,700 potential exoplanets since its launch in 2009, and scientists using the Kitt Peak National Observatory categorized the home stars of many of those planet candidates for the past three years. In particular, the researchers made detailed follow-up observations of 300 of the stars Kepler found likely to be harboring exoplanets.

The Kepler satellite, in orbit around the sun, stares at a region of the northern hemisphere sky sandwiched between the bright stars Vega and Deneb. Attached to the telescope is the largest imaging camera ever flown into space—16 million pixels—the only instrument on the telescope and the one used to monitor all the stars in its search for planets. Planets are detected if they pass in front of their parent sun, causing a very slight dip in the star’s brightness. When this dip repeats periodically, it reveals the presence of a possible planet, the length of the planet’s “year”, and other information.

One of the main findings of this initial work is that our observations indicate that most of the stars we observed are slightly larger than previously thought and one quarter of them are at least 35 percent larger,” astronomer and leader of the study Mark Everett said in a statement. “Therefore, any planets orbiting these stars must be larger and hotter as well. By implication, these new results reduce the number of candidate Earth-size planet analogues detected by Kepler.”

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Cosmic Dance: Creation of Supermassive Black Holes

Evolution of two equal sized galaxies colliding and forming a massive cloud of gas that will collapse into black hole.

Credit: Ohio State University

What Have We Learned About Pluto?

This month (March 2016), in the journal Science, New Horizons scientists have authored the first comprehensive set of papers describing results from last summer’s Pluto system flyby. These detailed papers completely transform our view of Pluto and reveal the former “astronomer’s planet” to be a real world with diverse and active geology, exotic surface chemistry, a complex atmosphere, puzzling interaction with the sun and an intriguing system of small moons.

Here’s a breakdown of what we’ve learned about Pluto:

1. Pluto has been geologically active throughout the past 4 billion years. The age-dating of Pluto’s surface through crater counts has revealed that Pluto has been geologically active throughout the past 4 billion years. Further, the surface of Pluto’s informally-named Sputnik Planum, a massive ice plain larger than Texas, is devoid of any detectable craters and estimated to be geologically young – no more than 10 million years old.

2. Pluto’s moon Charon has been discovered to have an ancient surface. As an example, the great expanse of smooth plains on Charon is likely a vast cryovolcanic flow or flows that erupted onto Charon’s surface about 4 billion years ago. These flows are likely related to the freezing of an internal ocean that globally ruptured Charon’s crust.

3. Pluto’s surface has many types of terrain. The distribution of compositional units on Pluto’s surface – from nitrogen-rich, to methane-rich, to water-rich – has been found to be surprisingly complex, creating puzzles for understanding Pluto’s climate and geologic history. The variations in surface composition on Pluto are unprecedented elsewhere in the outer solar system.

4. Pluto’s atmosphere is colder than we thought. Pluto’s upper atmospheric temperature has been found to be much colder (by about 70 degrees Fahrenheit) than had been thought from Earth-based studies, with important implications for its atmospheric escape rate. Why the atmosphere is colder is a mystery. 

5. We know what Pluto’s atmosphere is made of. The New Horizon spacecraft made observations of sunlight passing through Pluto’s atmosphere. We see absorption features that indicate an atmosphere made up of nitrogen (like Earth’s) with methane, acetylene and ethylene as minor constituents.

6. We might have an idea for how Pluto’s haze formed. For first time, a plausible mechanism for forming Pluto’s atmospheric haze layers has been found. This mechanism involves the concentration of haze particles by atmospheric buoyancy waves, created by winds blowing over Pluto’s mountainous topography. Pluto’s haze extends hundreds of kilometers into space, and embedded within it are over 20 very thin, but far brighter, layers.

7. There isn’t much dust around Pluto. Before the flyby, there was concern that a small piece of debris (even the size of a grain of sand) could cause great damage to (or even destroy) the spacecraft. But the Venetia Burney Student Dust Counter (an instrument on the New Horizons spacecraft) only counted a single dust particle within five days of the flyby. This is similar to the density of dust particles in free space in the outer solar system – about 6 particles per cubic mile – showing that the region around Pluto is, in fact, not filled with debris.

8. Pluto’s atmosphere is smaller than we expected. The uppermost region of Pluto’s atmosphere is slowly escaping to space. The hotter the upper atmosphere, the more rapid the gasses escape. The lower the planet’s mass, the lower the gravity, and the faster the atmospheric loss. As molecules escape, they are ionized by solar ultraviolet light. Once ionized, the charged molecules are carried away by the solar wind. As more Pluto-genic material is picked up by the solar wind, the more the solar wind is slowed down and deflected around Pluto. So - the net result is a region (the interaction region), which is like a blunt cone pointed toward the sun, where the escaping ionized gasses interact with the solar wind. The cone extends to a distance about 6 Pluto radii from Pluto toward the sun, but extend behind Pluto at least 400 Pluto radii behind Pluto - like a wake behind the dwarf planet.

9. Pluto’s moons are brighter than we thought. The high albedos (reflectiveness) of Pluto’s small satellites (moons) – about 50 to 80 percent – are entirely different from the much lower reflectiveness of the small bodies in the general Kuiper Belt population, which range from about 5 to 20 percent. This difference lends further support to the idea that these moons were not captured from the general Kuiper Belt population, but instead formed by the collection of material produced in the aftermath of the giant collision that created the entire Pluto satellite system.  

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