Unit Circle.

Strong words to use on a Resume

If you have ever had to write a resume for work or for an application, then you know the hardest part is figuring out what type of words to use that sound professional and and intelligent.

Example: If an application asks you if you have any relevant experience for a job at a day care center and you have experience, like you have babysat children. You would look at the words in the columns to see what words you should use that will help your resume stand out. You might put down “Have supervised and attended to children on a regular basis.”

I hope this is helpful to you.

Saturn’s hexagon

This colorful view from NASA’s Cassini mission is the highest-resolution view of the unique six-sided jet stream at Saturn’s north pole known as “the hexagon.” This movie, made from images obtained by Cassini’s imaging cameras, is the first to show the hexagon in color filters, and the first movie to show a complete view from the north pole down to about 70 degrees north latitude.

Via NASA: In Full View: Saturn’s Streaming Hexagon

is there anything you can tell us to expand on the space time ripples found in simulated black hole collisions?

Hi!

In one of my other responses I explained the whole concept of space time, here’s how i explained that:

A way that you can picture the bending of space time is this:

Picture two chairs, the backs facing each other. Then tape one end of a blanket to one of the chair backs and the other end of the blanket to the other chair back. What you have now should like this:

Now, if you were to place a tennis ball somewhere on the light blue blanket (top blanket), that blanket would no longer be flat, there would be a bend or a curve in it. Let’s say you put a basketball on the top blanket instead of a tennis ball. Since the basketball is bigger, the bend/curve that it makes will be a lot bigger than the tennis ball’s because the basketball has more mass.

So that blue blanket at the top of the chairs represents space time. If there were to be two large objects, let’s say basketballs, that were to “collide” (representing two black holes). Since they’re so large, they’d create these ripples in the blanket that can be observed.

Another easier way to think about it is like dropping a pebble into a lake. The bigger the pebble, the stronger and more frequent the ripples are. So since black holes are very massive, they create larger ripples compared to something smaller!

Astronomers haven’t been able to directly observe these ripples in space time, they were theorized by Einstein, however there’s an announcement being made all over the world today about data obtained from the Laser Interferometer Gravitational-Wave Observatory (LIGO)!

Here is a link talking a bit about that press conference!

I hope that helped to clarify everything! If not, feel free to ask again and I’ll try my best to clarify!

UPDATE: HERE are the findings of the conference, they’ve detected them for the first time!

Would It Be A Bad Thing to Wipe Out A Species … If It’s A Mosquito?

Mosquitoes have a nasty reputation.

The species Aedes aegypti, for example, is currently responsible for spreading the Zika virus through the Americas and also infects humans with dengue fever, chikungunya and yellow fever.

This raises the question: Should there be an effort to get rid of Aedes aegypti for good?

“There’s been lots of debate in the last 10 years whether we should eradicate mosquitoes, or at least the 100 species or so that serve as disease vectors for humans,” says David Magnus, director of Stanford University’s Center for Biomedical Ethics. “If you look at the science, the majority [of scientists] think we could probably eliminate mosquitoes without too much harm on the environment.”

Read the full story here.

Illustration: Matthew Twombly

The upper atmosphere of the Sun is dominated by plasma filled magnetic loops (coronal loops) whose temperature and pressure vary over a wide range. The appearance of coronal loops follows the emergence of magnetic flux, which is generated by dynamo processes inside the Sun. Emerging flux regions (EFRs) appear when magnetic flux bundles emerge from the solar interior through the photosphere and into the upper atmosphere (chromosphere and the corona). The characteristic feature of EFR is the Ω-shaped loops (created by the magnetic buoyancy/Parker instability), they appear as developing bipolar sunspots in magnetograms, and as arch filament systems in Hα. EFRs interact with pre-existing magnetic fields in the corona and produce small flares (plasma heating) and collimated plasma jets. The GIFs above show multiple energetic jets in three different wavelengths. The light has been colorized in red, green and blue, corresponding to three coronal temperature regimes ranging from ~0.8Mk to 2MK. 

Image Credit: SDO/U. Aberystwyth

at what point in history do you think americans stopped having british accents

Stellar Outburst Brings Water Snow Line Into View

ESO - European Southern Observatory logo. 13 July 2016

Artist’s impression of the water snowline around the young star V883 Orionis

The Atacama Large Millimeter/submillimeter Array (ALMA) has made the first ever resolved observation of a water snow line within a protoplanetary disc. This line marks where the temperature in the disc surrounding a young star drops sufficiently low for snow to form. A dramatic increase in the brightness of the young star V883 Orionis flash heated the inner portion of the disc, pushing the water snow line out to a far greater distance than is normal for a protostar, and making it possible to observe it for the first time. The results are published in the journal Nature on 14 July 2016.

ALMA image of the protoplanetary disc around V883 Orionis

Young stars are often surrounded by dense, rotating discs of gas and dust, known as protoplanetary discs, from which planets are born. The heat from a typical young solar-type star means that the water within a protoplanetary disc is gaseous up to distances of around 3 au from the star [1] — less than 3 times the average distance between the Earth and the Sun — or around 450 million kilometres [2]. Further out, due to the extremely low pressure, the water molecules transition directly from a gaseous state to form a patina of ice on dust grains and other particles. The region in the protoplanetary disc where water transitions between the gas and solid phases is known as the water snow line [3].

The star V883 Orionis in the constellation of Orion

But the star V883 Orionis is unusual. A dramatic increase in its brightness has pushed the water snow line out to a distance of around 40 au (about 6 billion kilometres or roughly the size of the orbit of the dwarf planet Pluto in our Solar System). This huge increase, combined with the resolution of ALMA at long baselines [4], has allowed a team led by Lucas Cieza (Millennium ALMA Disk Nucleus and Universidad Diego Portales, Santiago, Chile) to make the first ever resolved observations of a water snow line in a protoplanetary disc.

Shifting water snowline in V883 Orionis

The sudden brightening that V883 Orionis experienced is an example of what occurs when large amounts of material from the disc surrounding a young star fall onto its surface. V883 Orionis is only 30% more massive than the Sun, but thanks to the outburst it is experiencing, it is currently a staggering 400 times more luminous — and much hotter [5].

ALMA image of the protoplanetary disc around V883 Orionis (annotated)

Lead author Lucas Cieza explains: “The ALMA observations came as a surprise to us. Our observations were designed to look for disc fragmentation leading to planet formation. We saw none of that; instead, we found what looks like a ring at 40 au. This illustrates well the transformational power of ALMA, which delivers exciting results even if they are not the ones we were looking for.”

ALMA image of the protoplanetary disc around V883 Orionis

The bizarre idea of snow orbiting in space is fundamental to planet formation. The presence of water ice regulates the efficiency of the coagulation of dust grains — the first step in planet formation. Within the snow line, where water is vapourised, smaller, rocky planets like our own are believed to form. Outside the water snow line, the presence of water ice allows the rapid formation of cosmic snowballs, which eventually go on to form massive gaseous planets such as Jupiter.

Zooming on the protoplanetary disc around V883 Orionis

The discovery that these outbursts may blast the water snow line to about 10 times its typical radius is very significant for the development of good planetary formation models. Such outbursts are believed to be a stage in the evolution of most planetary systems, so this may be the first observation of a common occurrence. In that case, this observation from ALMA could contribute significantly to a better understanding of how planets throughout the Universe formed and evolved.

The protoplanetary disc around V883 Orionis (artist’s impression)

Notes: [1] 1 au, or one astronomical unit, is the mean distance between the Earth and the Sun, around 149.6 million kilometres.This unit is typically used to describe distances measured within the Solar System and planetary systems around other stars. [2] This line was between the orbits of Mars and Jupiter during the formation of the Solar System, hence the rocky planets Mercury, Venus, Earth and Mars formed within the line, and the gaseous planets Jupiter, Saturn, Uranus and Neptune formed outside. [3] The snow lines for other molecules, such as carbon monoxide and methane, have been observed previously with ALMA, at distances of greater than 30 au from the protostar within other protoplanetary discs. Water freezes at a relatively high temperature and this means that the water snow line is usually much too close to the protostar to observe directly. [4] Resolution is the ability to discern that objects are separate. To the human eye, several bright torches at a distance would seem like a single glowing spot, and only at closer quarters would each torch be distinguishable. The same principle applies to telescopes, and these new observations have exploited the exquisite resolution of ALMA in its long baseline modes. The resolution of ALMA at the distance of V883 Orionis is about 12 au — enough to resolve the water snow line at 40 au in this outbursting system, but not for a typical young star. [5] Stars like V883 Orionis are classed as FU Orionis stars, after the original star that was found to have this behaviour. The outbursts may last for hundreds of years. More information: This research was presented in a paper entitled “Imaging the water snow-line during a protostellar outburst”, by L. Cieza et al., to appear in Nature on 14 July 2016. The team is composed of Lucas A. Cieza (Millennium ALMA Disk Nucleus; Universidad Diego Portales, Santiago, Chile), Simon Casassus (Universidad de Chile, Santiago, Chile), John Tobin (Leiden Observatory, Leiden University, The Netherlands), Steven Bos (Leiden Observatory, Leiden University, The Netherlands), Jonathan P. Williams (University of Hawaii at Manoa, Honolulu, Hawai`i, USA), Sebastian Perez (Universidad de Chile, Santiago, Chile), Zhaohuan Zhu (Princeton University, Princeton, New Jersey, USA), Claudio Cáceres (Universidad Valparaiso, Valparaiso, Chile), Hector Canovas (Universidad Valparaiso, Valparaiso, Chile), Michael M. Dunham (Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts, USA), Antonio Hales (Joint ALMA Observatory, Santiago, Chile), Jose L. Prieto (Universidad Diego Portales, Santiago, Chile), David A. Principe (Universidad Diego Portales, Santiago, Chile), Matthias R. Schreiber (Universidad Valparaiso, Valparaiso, Chile), Dary Ruiz-Rodriguez (Australian National University, Mount Stromlo Observatory, Canberra, Australia) and Alice Zurlo (Universidad Diego Portales & Universidad de Chile, Santiago, Chile). The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of ESO, the U.S. National Science Foundation (NSF) and the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Republic of Chile. ALMA is funded by ESO on behalf of its Member States, by NSF in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and by NINS in cooperation with the Academia Sinica (AS) in Taiwan and the Korea Astronomy and Space Science Institute (KASI). ALMA construction and operations are led by ESO on behalf of its Member States; by the National Radio Astronomy Observatory (NRAO), managed by Associated Universities, Inc. (AUI), on behalf of North America; and by the National Astronomical Observatory of Japan (NAOJ) on behalf of East Asia. The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA. ESO is the foremost intergovernmental astronomy organisation in Europe and the world’s most productive ground-based astronomical observatory by far. It is supported by 16 countries: Austria, Belgium, Brazil, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Poland, Portugal, Spain, Sweden, Switzerland and the United Kingdom, along with the host state of Chile. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world’s most advanced visible-light astronomical observatory and two survey telescopes. VISTA works in the infrared and is the world’s largest survey telescope and the VLT Survey Telescope is the largest telescope designed to exclusively survey the skies in visible light. ESO is a major partner in ALMA, the largest astronomical project in existence. And on Cerro Armazones, close to Paranal, ESO is building the 39-metre European Extremely Large Telescope, the E-ELT, which will become “the world’s biggest eye on the sky”. Links: Research paper: http://www.eso.org/public/archives/releases/sciencepapers/eso1626/eso1626a.pdf Photos of ALMA: http://www.eso.org/public/images/archive/search/?adv=&subject_name=Atacama%20Large%20Millimeter/submillimeter%20Array For more information about ALMA, visit: https://www.eso.org/sci/facilities/alma.html Images, Text, Credits: ESO/Richard Hook/A. Angelich (NRAO/AUI/NSF)/ALMA (ESO/NAOJ/NRAO)/ALMA//L. Cieza/IAU and Sky & Telescope/Videos: ALMA (ESO/NAOJ/NRAO)/L. Cieza./ESO/Digitized Sky Survey 2/N. Risinger (skysurvey.org)/M. Kornmesser. Music: Johan B. Monell. Best regards, Orbiter.ch Full article

Science When the Sun Don’t Shine

About once a year, somewhere on Earth, the sun is blocked by the moon. This phenomenon – called a total solar eclipse – is one of the most beautiful natural events.

Blocking the light of the sun during a total solar eclipse reveals the sun’s relatively faint, feathery atmosphere, called the corona. The corona is one of the most interesting parts of the sun. We usually study it using an instrument called a coronagraph, which uses a solid disk to make an artificial eclipse by blocking the sun’s face.

To successfully block all of the sun’s bright light – which can bend around the sharp edges of a coronagraph disk – coronagraphs must block much more than just the face of the sun.  So total solar eclipses are a rare chance to study the lower part of the corona, close to the surface of the sun.   

We have sent a team of scientists to Indonesia, where they’re preparing for an experiment during the March 8, 2016, eclipse, visible from Southeast Asia.

The scientists are measuring a certain kind of light – called polarized light – scattered by electrons in the lower corona, which will help us understand the temperature and speed of these electrons.

The March 8 eclipse is a preview of the total solar eclipse that will be visible across the US in August 2017.

Remember, you should never look directly at the sun – even if the sun is partly obscured. This also applies during a total eclipse up until the time when the sun is completely and totally blocked. More on safety: http://go.nasa.gov/1L6xpnI

For more eclipse information, check out nasa.gov/eclipse

Make sure to follow us on Tumblr for your regular dose of space: http://nasa.tumblr.com

Volcanic ash being hit by sunset. This is Volcán Puyehue, in Chile.

Colourised footage of Benjamin, the last know Tasmanian Tiger (Thylacine).

Benjamin died on September 7th, 1936 in Hobart zoo. It is believed that he died out of neglect, as he was locked out of his shelter and was exposed to the searing hot sun and freezing cold night of Tasmania.

The Thylacine was one of the last large marsupials left on Australia (the other being the Kangaroo) after a great extinction event occurred around 40 thousand years ago. This extinction event, caused mainly by the arrival of humans, wiped out 90% of Australia’s terrestrial vertebrates, including the famous Megafauna.

The Thylacine was around 15-30kg (33-66lbs), were carnivorous, and had numerous similarities to other species like dogs, despite not being related and purely by chance, in a phenomenon known as convergent evolution (just like the ability to fly of bats and birds, despite following different evolutionary paths). Not only that, they could open their jaws up to 120 degrees, could hop around on two legs like a kangaroo, and both males and females had pouches.

Lastly in a cruel twist, the Tasmanian government decided to protect the Thylacine - just 59 days before the last one died, in a very notable case case of “Too little too late”. To date, many biologists believe that there are still Thylacine roaming the wild plains of Australia.