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May 2016 ~ Worm 4 Space

Tuesday 24 May 2016

Richard Feynman

Richard Feynman  : was a Nobel Prize-winning American physicist, particularly known for his contributions to quantum physics, quantum electrodynamics and particle physics, as well as quantum computing and nanotechnology. During his lifetime, he was one of the best-known scientists in the world, and was a great popularizer of physics through his books and lectures. He was also regarded as something of an eccentric and free spirit, and brought a wicked sense of humour to his work, as exemplified by his well-known quote “I think I can safely say that nobody understands quantum mechanics”.

Richard Phillips Feynman was born on 11 May 1918 in Queens, New York to Jewish parents originally from Russia and Poland. As a child, he was heavily influenced by both his father, Melville, who encouraged him to ask questions to challenge orthodox thinking, and his mother, Lucille, from whom he inherited the sense of humour that he maintained throughout his life. His sister Joan also became a professional physicist.
By his early youth, Feynman described himself as an "avowed atheist". He delighted in repairing radios and demonstrated a talent for engineering from an early age. At Far Rockaway High School in Queens, he excelled in mathematics, and won the New York University Math Championship by a large margin in his final year there.
He was refused entry to his first choice Columbia University because of the "Jewish quota" and attended instead the Massachusetts Institute of Technology, where he received a bachelor's degree in 1939, and was named a Putnam Fellow. He obtained an unprecedented perfect score on the graduate school entrance exams to Princeton University (although he did rather poorly on the history and English portions), where he went to study mathematics and physics along with other luminaries such as Albert EinsteinWolfgang Pauli and John von Neumann. He received a PhD from Princeton in 1942, under his advisor John Wheeler, with a thesis in which he developed an approach to quantum mechanics governed by the principle of “least action”, replacing the wave-oriented electromagneticpicture developed by James Clerk Maxwell with one based entirely on particle interactions mapped in space and time.
During his time at Princeton, he married his first wife, Arline Greenbaum, although she died of tuberculosis just a few years later in 1945. A second marriage, in June 1952, to Mary Louise Bell, was brief and unsuccessful.
While at Princeton, Feynman was persuaded by the physicist Robert Wilson to participate in the Manhattan Project, the wartime US Army project at Los Alamos to develop an atomic bomb. Although not central to the project, he immersed himself in this work, and was soon made a group leader under Hans Bethe, and was present at the Trinity bomb test in 1945. As part of the project, he assisted in establishing the system for using IBM punched cards for computation, and in calculating neutronequations for nuclear reactors. Later, at the US Army’s Oak Ridge facility, he devised safety procedures for atomic material storage, and did theoretical work on the proposed uranium-hydride bomb, which later proved not to be feasible. He also gained a reputation for his pranks and practical jokes, and for his habit of Indian-style drumming out in the desert.
During his time at Los Alamos, Niels Bohr sought him out for discussions about physics, and he became a close friend of laboratory head Robert Oppenheimer, who unsuccessfully tried to lure him to the University of California in Berkeley after the war. Looking back, Feynman thought his decision to work on the Manhattan Project was justified at the time, but expressed grave reservations about the continuation of the project after the defeat of Nazi Germany, and suffered bouts of depression after the destruction of Hiroshima.
After the war, Feynman declined an offer from the Institute for Advanced Study in Princeton, New Jersey, despite the presence there of such distinguished faculty members as Albert Einstein, Kurt Gödel and John von Neumann. Instead he followed Hans Bethe to Cornell University, where he taught theoretical physics from 1945 to 1950. Feynman then opted for the position of Professor of Theoretical Physics at the California Institute of Technology (partly for the climate, as he admits), despite offers of professorships from other renowned universities. He remained there for the rest of his career.
In California, he married for the third time, to an English woman called Gweneth Howarth who shared his enthusiasm for life and spirited adventure. In 1962, they had a son, Carl, and adopted a daughter, Michelle, in 1968. Carl inherited his father’s love of, and propensity for, mathematics and went on to work at a high level in the computer field, particularly in the use of multiple computers to solve complex problems, later known as parallel computing.
Feynman gained a reputation for being able to explain complex elements of theoretical physics in an easily understandable way, and was sometimes referred to as “The Great Explainer”. He opposed rote learning or unthinking memorization, although he could also be strict with unprepared students. His 1964 book “Feynman Lectures On Physics”, which includes lectures on mathematics,electromagnetism, Newtonian physics, quantum physics and even the relation of physics to other sciences, remains a classic. Other lectures and miscellaneous talks were also turned into books, including “The Character of Physical Law”, “QED: The Strange Theory of Light and Matter”, “Statistical Mechanics” and “Lectures on Gravity”.
In December 1959, Feynman gave a visionary and ground-breaking talk entitled "There's Plenty of Room at the Bottom" at an American Physical Society meeting at the California Institute of Technology. In it, he suggested the possibility of building structures one atom or molecule at a time, an idea which seemed fantastic at the time, but which has since become widely known as nanotechnology. He personally offered $1,000 prizes for two of his challenges in nanotechnology, which were claimed by William McLellan and Tom Newman.
He was also one of the first scientists to conceive of the possibility of quantum computers and played a crucial role in developing the first massively parallel computer, finding innovative uses for it in numerical computations, building neural networks and physical simulations using cellular automata.
During his years at Caltech, he worked on, among other things: quantum electrodynamics (the theory of the interaction between light and matter) which he had begun developing at Cornell, and for which he was awarded the 1965 Nobel Prize in Physics jointly with Julian Schwinger and Sin-Itiro Tomonaga; the physics of the superfluidity of supercooled liquid helium and its quantum mechanical behaviour; a model of weak decay (such as the decay of a neutron into an electron, a proton and an anti-neutrino) in collaboration with fellow CalTech professor Murray Gell-Mann; his parton model for analyzing high-energy hadron collisions, which he developed in parallel with Murray Gell-Man’s theory of quarks(although the quark model would be the one to gain general acceptance).
In his work on quantum electrodynamics, he developed an important tool known as Feynman diagrams to help conceptualize and calculate interactions between particles in space-time, notably the interactions between electrons and their anti-matter counterparts, positrons. Feynman diagrams, which are easily-visualized graphic analogues of the complicated mathematical expressions needed to describe the behaviour of systems of interacting particles, have permeated many areas of theoretical physics in the second half of the 20th Century. His ambitious idea was to use the diagrams to model all of physics in terms of particles' spins and fundamental forces, and to explain the strong interactions governing the scattering of nucleons.
He was appointed a foreign member of the Royal Society in 1965, and later won the Oersted Medal for teaching, of which he seemed especially proud. He also became a member of the American Physical Society, the American Association for the Advancement of Science and the National Academy of Science. Later in life, Feynman turned his mind to theories of quantum gravity. Although not developed for the purpose, his Feynman diagrams had became fundamental for developing string theory and M-theory. He was not, however, totally convinced by the theories, and criticized string theorists for “not calculating anything” and for not checking their ideas.
Just two years before his death, Feynman played an important role in the Rogers Commission investigation of the 1986 Challenger Space Shuttle disaster. He developed two rare forms of cancer, Liposarcoma and Waldenström's macroglobulinemia, and died on 15 February 1988 in Los Angeles, shortly after a final attempt at surgery for the former. His last recorded words are noted as “I'd hate to die twice. It's so boring.”

Saturday 21 May 2016

NASA : Bigelow Expandable Activity Module


Concept image of the Bigelow Expandable Activity Module (BEAM)
This artist's concept depicts the Bigelow Expandable Activity Module (BEAM), constructed by Bigelow Aerospace, attached to the International Space Station (ISS). The BEAM will be launched to the space station later this year.
Credits: Bigelow Aerospace
The Bigelow Expandable Activity Module (BEAM) is an expandable habitat technology demonstration for the International Space Station. Expandable habitats greatly decrease the amount of transport volume for future space missions. These “expandables” are lightweight and require minimal payload volume on a rocket, but expand after being deployed in space to potentially provide a comfortable area for astronauts to live and work. They also provide a varying degree of protection from solar and cosmic radiation, space debris, atomic oxygen, ultraviolet radiation and other elements of the space environment. 
The journey to Mars is complex and filled with challenges that NASA and its partners are continuously working to solve. Before sending the first astronauts to the Red Planet, several rockets filled with cargo and supplies will be deployed to await the crews’ arrival. Expandable modules, which are lower-mass and lower-volume systems than metal habitats, can increase the efficiency of cargo shipments, possibly reducing the number of launches needed and overall mission costs.
Mission Highlights
  • BEAM is scheduled to launch on the eighth SpaceX Commercial Resupply Service mission. After being attached to the Tranquility Node using the station’s robotic Canadarm2, it will be filled with air to expand it for a two-year test period in which astronauts aboard the space station will conduct a series of tests to validate overall performance and capability of expandable habitats.
  • Crews will routinely enter to take measurements and monitor its performance to help inform designs for future habitat systems. Learning how an expandable habitat performs in the thermal environment of space and how it reacts to radiation, micrometeroids, and orbital debris will provide information to address key concerns about living in the harsh environment of space.
  • Following the two-year test and validation period, BEAM will be robotically jettisoned from the space station, leaving orbit to burn during its descent through Earth’s atmosphere—much like many cargo spacecraft do.
  • If BEAM performs favorably, it could lead to future development of expandable habitation structures for future crews traveling in deep space.
  • The BEAM is an example of NASA’s increased commitment to partnering with industry to enable the growth of the commercial use of space. The BEAM project is co-sponsored by NASA's Advanced Exploration Systems (AES) Division and Bigelow Aerospace, which pioneers innovative approaches to rapidly and affordably develop prototype systems for future human exploration missions. The BEAM demonstration supports an AES objective to develop a deep space habitat for human missions beyond Earth orbit. 

More about BEAM

Sunday 15 May 2016

The WMAP

Wilkinson Microwave Anisotropy Probe :


From Wikipedia, the free encyclopedia
"WMAP" redirects here. WMAP may also refer to either radio station WXNC or WGSP-FM.
Wilkinson Microwave Anisotropy Probe
WMAP spacecraft.jpg
Artist's impression of WMAP
NamesMAP
Explorer 80
Mission typeCMBR Astronomy
OperatorNASA
COSPAR ID2001-027A
SATCAT №26859
Websitemap.gsfc.nasa.gov
Mission duration9 years, 1 month, 19 days
Spacecraft properties
ManufacturerNASA / NRAO
Launch mass835 kg (1,841 lb)[1]
Dry mass763 kg (1,682 lb)
Dimensions3.6 m × 5.1 m (12 ft × 17 ft)
Power419 W
Start of mission
Launch date19:46:46, June 30, 2001[2]
RocketDelta II 7425-10
Launch siteCape Canaveral SLC-17
End of mission
Disposalpassivated
DeactivatedOctober 28, 2010
Orbital parameters
Reference systemL2 point
RegimeLissajous
Main telescope
TypeGregorian
Diameter1.4 m × 1.6 m (4.6 ft × 5.2 ft)
Wavelengths23 GHz to 94 GHz
Instruments
WMAP collage.jpg
NASA collage of WMAP-related imagery (spacecraft, CMB spectrum and background image)

Explorers program
← HETERHESSI →
The Wilkinson Microwave Anisotropy Probe (WMAP), originally known as the Microwave Anisotropy Probe(MAP) was a spacecraft operating from 2001 to 2010 which measured differences across the sky in the temperature of the cosmic microwave background (CMB) – the radiant heat remaining from the Big Bang.[3][4] Headed by ProfessorCharles L. Bennett of Johns Hopkins University, the mission was developed in a joint partnership between the NASAGoddard Space Flight Center and Princeton University.[5] The WMAP spacecraft was launched on June 30, 2001 from Florida. The WMAP mission succeeded the COBE space mission and was the second medium-class (MIDEX) spacecraft in the NASA Explorers program. In 2003, MAP was renamed WMAP in honor of cosmologist David Todd Wilkinson(1935–2002),[5] who had been a member of the mission's science team. After 9 years of operations, WMAP was switched off in 2010, following the launch of the more advanced Planck spacecraft by ESA in 2009.
WMAP's measurements played a key role in establishing the current Standard Model of Cosmology: the Lambda-CDM model. The WMAP data are very well fit by a universe that is dominated by dark energy in the form of a cosmological constant. Other cosmological data are also consistent, and together tightly constrain the Model. In the Lambda-CDM model of the universe, the age of the universe is 13.772±0.059 billion years. The WMAP mission's determination of the age of the universe to better than 1% precision was recognized by the Guinness Book of World Records.[6] The current expansion rate of the universe is (see Hubble constant) of 69.32±0.80 km·s−1·Mpc−1. The content of the universe presently consists of 4.628%±0.093% ordinary baryonic matter24.02%+0.88%
−0.87%
 Cold dark matter (CDM) that neither emits nor absorbs light; and 71.35%+0.95%
−0.96%
 of dark energy in the form of a cosmological constant that accelerates the expansion of the universe.[7] Less than 1% of the current contents of the universe is in neutrinos, but WMAP's measurements have found, for the first time in 2008, that the data prefers the existence of a cosmic neutrino background[8] with an effective number of neutrino species of 3.26±0.35. The contents point to a Euclidean flat geometry, with curvature (\Omega_{k}) of −0.0027+0.0039
−0.0038
. The WMAP measurements also support the cosmic inflationparadigm in several ways, including the flatness measurement.
The mission has won various awards: according to Science magazine, the WMAP was the Breakthrough of the Year for 2003.[9] This mission's results papers were first and second in the "Super Hot Papers in Science Since 2003" list.[10] Of the all-time most referenced papers in physics and astronomy in the INSPIRE-HEP database, only three have been published since 2000, and all three are WMAP publications. Bennett, Lyman A. Page, Jr., and David N. Spergel, the latter both of Princeton University, shared the 2010 Shaw Prize in astronomy for their work on WMAP.[11] Bennett and the WMAP science team were awarded the 2012 Gruber Prize in cosmology.
As of October 2010, the WMAP spacecraft is derelict in a heliocentric graveyard orbit after 9 years of operations.[12] All WMAP data are released to the public and have been subject to careful scrutiny. The final official data release was thenine-year release in 2012.[13][14]
Some aspects of the data are statistically unusual for the Standard Model of Cosmology. For example, the largest angular-scale measurement, the quadrupole moment, is somewhat smaller than the Model would predict, but this discrepancy is not highly significant.[15] A large cold spot and other features of the data are more statistically significant, and research continues into these.

Thursday 12 May 2016

Big Bounce

The Big Bounce: The big bang may not have been the beginning of the universe, but merely the beginning of one of an infinite series of universes. Yeah, wrap your mind around that!Courtesy Pat Rawlings/SAICThe Big Bang and the new kid - the Big Bounce - are facing off and it looks as if the Big Bounce is pulling ahead in the polls. Big bounce theory, proposed by Martin Bojowald, is based on loop quantum gravity. And what, you may ask, is loop quantum gravity??
Well, since you asked so nicely...loop quantum gravity - or loop gravity - is a theory of spacetime that attempts to reconcile quantum mechanics and general relativity, according to Wikipedia. Basically, loop gravity tries to prove that gravity is quantized (or broken down into discrete steps). Read more here.
So now that you know a little bit about loop gravity, we can move on to the theory at hand. The big bounce says that the universe is like a bouncy ball. When the ball hits the ground, the universe is at its smallest; as the ball rises above the ground, the universe expands; as the ball moves back towards the ground, the universe begins to implode; when the ball starts to rise after hitting the ground, the universe expands again... You get the idea.
Where the big bounce differs from the big bang is that it resolves the issue of the big bang singularity. And again, you may ask, what in the world is the big bang singularity? Well, for those of you not in the know: the big bang singularity is the single point from which the entire universe is supposed to have sprung. It is, in fact, the major sticking point in the big bang theory; the calculations just can't account for such a singularity.
So for years, this singularity has been an assumption inherent in the theory. And you know what the problem with assuming is...
This is where the big bounce starts to look mighty good! The big bounce suggests that, as the universe implodes, the energy density of space increases to a point that gravity ceases to be attractive and repulses instead. When gravity becomes repulsive, the universe stops shrinking and begins to expand. Once the density moderates, gravity switches back to being attractive. This explains the explosive expansion seen and accounted for in the big bang theory.Big Bounce: The universe implodes until gravity becomes repulsive and a new universe explodes from the ashes, so to speak.Courtesy Relativity 4 Engineers
Now here is where the big bounce gets really cool! The idea that the universe implodes and explodes like a ball bouncing leads Bojowald to believe that there have been an infinite number of universes before ours and an infinite number of universes to come. Each universe expands, increasing in inertia (or disorder) until it implodes, thus clearing the slate for the new universe.

Sunday 8 May 2016

NASA : Satellites to See Mercury Enter Spotlight on May 9


By NASA 
It happens only a little more than once a decade – and the next chance to see it is Monday, May 9. Throughout the U.S., sky watchers can watch Mercury pass between Earth and the sun in a rare astronomical event known as a planetary transit. Mercury will appear as a tiny black dot as it glides in front of the sun’s blazing disk over a period of seven and a half hours. Three NASA satellites will be providing images of the transit and one of them will have a near-live feed.



Although Mercury zooms around the sun every 88 days, Earth, the sun and Mercury rarely align. And because Mercury orbits in a plane that is tilted from Earth’s orbit, it usually moves above or below our line of sight to the sun. As a result, Mercury transits occur only about 13 times a century.
Transits provide a great opportunity to study the way planets and stars move in space – information that has been used throughout the ages to better understand the solar system and which still helps scientists today calibrate their instruments. Three of NASA's solar telescopes will watch the transit for just that reason.
The May 9 Mercury transit will occur between about 7:12 a.m. and 2:42 p.m. EDT. Mercury is too small to see without magnification, but it can be seen with a telescope or binoculars. These must be outfitted with a solar filter as you can't safely look at the sun directly.
“Astronomers get excited when any two things come close to each other in the heavens,” said Louis Mayo, program manager at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “This is a big deal for us.”
Mercury transits have been key to helping astronomers throughout history: In 1631, astronomers first observed a Mercury transit. Those observations allowed astronomers to measure the apparent size of Mercury’s disk, as well as help them estimate the distance from Earth to the sun.
“Back in 1631, astronomers were only doing visual observations on very small telescopes by today’s standards,” said Mayo.
Since then, technological advancements have allowed us to study the sun and planetary transits in greater detail. In return, transits allow us to test our spacecraft and instruments.
Scientists for the Solar and Heliospheric Observatory, or SOHO (jointly operated by NASA and ESA, the European Space Agency), and NASA’sSolar Dynamics Observatory, or SDO, will work in tandem to study the May 9 transit. The Hinode solar mission will also observe the event. Hinode is a collaboration between the space agencies of Japan, the United States, the United Kingdom and Europe led by the Japan Aerospace Exploration Agency.

SOHO launched in December 1995 with 12 instruments to study the sun from the deep solar core all the way out to the sun's effects on the rest of the solar system. Two of these instruments — the Extreme ultraviolet Imaging Telescope and the Michelson Doppler Imager — will be brought back into full operation to take measurements during the transit after five years of quiescence.
For one thing, the SOHO will measure the sun’s rotation axis using images captured by the spacecraft.
“Instruments on board SDO and SOHO use different spectral lines, different wavelengths and they have slightly different optical properties to study solar oscillations,” said SOHO Project Scientist Joseph Gurman. “Transit measurements will help us better determine the solar rotation axis.”
Such data is another piece of a long line of observations, which together help us understand how the sun changes over hours, days, years and decades.
“It used to be hard to observe transits,” Gurman said. “If you were in a place that had bad weather, for example, you missed your chance and had to wait for the next one. These instruments help us make our observations, despite any earthly obstacles.”
SDO will be able to use the transit to help with instrument alignment. Because scientists know so precisely where Mercury should be in relationship to the sun, they can use it as a marker to fine tune exactly how their instruments should be pointed.
The transit can also be used to help calibrate space instruments. The utter darkness of the planet provides an opportunity to study effects on the observations of stray light within the instrument. The backside of Mercury should appear black as it moves across the face of the sun. But because instruments scatter some light, Mercury will look slightly illuminated.
“It’s like getting a cataract — you see stars or halos around bright lights as though you are looking through a misty windshield,” said SDO Project Scientist Dean Pesnell. “We have the same problem with our instruments.”
Scientists run software on the images to try and mitigate the effect and check whether it can remove all of the scattered light.
For those of us down on the ground, it is worth trying to find a local astronomy club with a solar telescope to see if you can witness this rare event.  Alternatively, a near-live feed of SDO images will be available at www.nasa.gov/transit.

Saturday 7 May 2016

Evolutionary Theory (Part 1)

Evolution is change in the heritable traits of biological populations over successive generations. Evolutionary processes give rise to diversity at every level of biological organisation, including the levels of species, individual organisms, andmolecules.
All life on Earth shares a common ancestor known as the last universal ancestor, which lived approximately 3.5–3.8 billion years ago, although a study in 2015 found "remains of biotic life" from 4.1 billion years ago in ancient rocks inWestern Australia.(by wikipedia).
Brief History of Evolutionary Theory Before Darwin :