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The color-magnitude diagram of notable stars. The brightest red supergiant, Betelgeuse, is shown at the upper right.
European Southern Observatory4:07 PM: See, there's nothing to be afraid of, here. Emily is telling us how stars, in general work, and it's nice and simple and straightforward. You burn through your fuel when you're on the main sequence, or this big streaky diagonal line. As you burn enough fuel and run out of hydrogen in your core, you evolve off of this line, towards the right (and up), and that's when you enter the red giant or supergiant phase. and that's where the fun begins.
The Sun, today, is very small compared to giants, but will grow to the size of Arcturus in its red giant phase. A monstrous supergiant like Antares will be forever beyond our Sun's reach. Ableton exit full screen mode mac. Adobe cc 2018 mac download.
English Wikipedia author Sakurambo4:09 PM: It's true: when you become a star like this, you become very different from how the Sun is now. But this doesn't mean you're 'weird' in any real way. it means you're obeying your normal phase of stellar evolution. And that's only weird from the perspective of normalizing us. In reality, there's a wide variety of what 'normal' is. Perhaps we should learn that stellar lesson for ourselves, at the moments where we feel we're not normal: there's a wide variety of what normal looks like.
The Omega nebula, known also as Messier 17, is an intense and active region of star formation, viewed edge-on, which explains its dusty and beam-like appearance.
ESO / VST survey4:13 PM: What's fun about stars and stellar evolution is that these very massive stars, the ones that become the red supergiants, are actually the shortest-lived of all stars. We find them even in star-forming regions, as they've burn through their hydrogen fuel in their core so fast, and when they expand, they cool, so drastically that they can actually form stable molecules (like titanium dioxide) in their outer atmospheres.
O-stars, the hottest of all stars, actually have weaker absorption lines in many cases, because the surface temperatures are great enough that most of the atoms at its surface are at too great of an energy to display the characteristic atomic transitions that result in absorption. Fertigen metin2 p server download internet explorer 1.
NOAO/AURA/NSF, modified by E. Siegel4:16 PM: What's interesting is that these stellar atmospheres are so large and so cool, that the molecules forming at the edges can absorb blue light, preferentially, which shift the fitted temperatures of these stars to values that were too low: in theory, stars that were too cool to exist. It's an interesting study in how we can fool ourselves if we don't account for all the physical effects, including, oddly, molecules on the surfaces of stars!
The anatomy of a very massive star throughout its life, culminating in a Type II Supernova when the core runs out of nuclear fuel. The final stage of fusion is silicon-burning, producing iron and iron-like elements in the core for only a brief while before a supernova ensues.
Nicole Rager Fuller/NSF4:20 PM: Okay, so how do you go through stellar evolution, and go supernova? To hold up your star against gravitational collapse, you have to fuse elements: the outward push of radiation fights gravity. When you run out of hydrogen to fuse, radiation starts to lose, and gravitational collapse happens. Video editin apps mac osx. That means, though, that you heat up as you get compressed, and if you have enough mass, you can heat up fast enough to start fusing helium.
This goes on: you fuse helium into carbon, carbon into oxygen. all the way up until you make iron, nickel, and cobalt. And then, my friend, you die.
4:23 PM: This is fast: while these different stages of burning last from days (like silicon) to thousands of years (for carbon/oxygen) to hundreds of thousands (for helium). but supernovae occur in seconds.
Ejecta from the eruption of the star V838 Monocerotis. Download metal gear solid psx iso psp free.
NASA, ESA and H.E. Bond (STScI)4:26 PM: But not everything is smooth like you think of. Emily's now telling us about luminous blue variables, which throw off ejecta as they go through their late-stages in life. This is an interesting process that isn't fully understood: why do some stars (usually the ones with more heavy elements) do this, while others don't? This kind of open question is part of why astronomy and astrophysics, despite all we know, is nowhere close to coming to an end! https://isrzfyd.weebly.com/fender-special-edition-custom-telecaster-fmt-hh-reviews.html.
A neutron star is one of the densest collections of matter in the Universe, but there is an upper limit to their mass. Exceed it, and the neutron star will further collapse to form a black hole.
ESO/Luís Calçada4:30 PM: The tough thing about a public talk like this is when you do a survey of objects or phenomena, you can't go too far in-depth into anything. Emily talked about neutron stars and specifically the ones that are pulsars, but then went right on to black holes. Why? Because if you want to cover it all, you can't spend too much time talking about any one thing in particular. There are, as a result, going to be lots of questions that flash through your mind, and then are lost as you go onto your next topic.
An illustration of a very high energy process in the Universe: a gamma-ray burst.
NASA / D. Berry4:32 PM: But on the other hand, it's also really cool, because you get to have a great survey of a whole slew of topics, like gamma-ray bursts. which we know now, thanks to LIGO/Virgo, are at least partially due to neutron star mergers!
4:35 PM: Here's something that you don't often get to appreciate in science: when you detect a rare or important event, here's the process for how it works.
- You get a notification that something interesting and timely occurred.
- People get kicked off of their observation runs, and the big/important telescopes turn to point at what you're seeking to detect.
- These follow-up observations, across a variety of wavelengths, give you a slew of data to look at.
- And it's the data, not a pretty picture, that tells you the interesting physics/astrophysics/astronomy that's going on.
And finally, you don't announce it, you post your results in a publication and then the community synthesizes the suite of what all the astronomers have to determine exactly what went on.
The galaxy NGC 4993, located 130 million light years away, had been imaged many times before. But just after the August 17, 2017 detection of gravitational waves, a new transient source of light was seen: the optical counterpart of a neutron star-neutron star merger.
P.K. Blanchard / E. Berger / Pan-STARRS / DECam4:38 PM: This is really a vital part of the process: being careful and making sure you're seeing what you think you're seeing. Science isn't always about being first or fastest or the one who puts all the pieces together; it's about learning as much as possible and getting it right in the end. It's how we combined gravitational wave astronomy, gamma-ray astronomy, and then multiwavelength follow-ups across over 70 observatories.
Aerial view of the Virgo gravitational-wave detector, situated at Cascina, near Pisa (Italy). Virgo is a giant Michelson laser interferometer with arms that are 3 km long, and complements the twin 4 km LIGO detectors.
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Nicola Baldocchi / Virgo Collaboration4:41 PM: I have to say, by the way, how exciting it is to see a pure astronomer like Emily, not an astrophysicist but an astronomer, talking about gravitational wave astronomy. Castle crasher exp glitch after patch. That's right, something that was once purely in the realm of physics, and then astrophysics, has made it to the point where astronomers talk about this as actual astronomy. This isn't just physics anymore; astronomers no longer need telescopes to do astronomy!
4:43 PM: By the way, it's important that Emily talks about these sensitive, transient events that are happening quickly, as time-domain astronomy. In other words, when time is of the essence, you absolutely have to look, because if you don't jump at your chance to take that data, you'll miss it!
A solar flare, visible at the right of the image, occurs when magnetic field lines split apart and reconnect, far more rapidly than prior theories have predicted.
NASA4:45 PM: Also, it's important to recognize that sometimes there are false positives. For example, potassium-flare stars. Who sees stars flaring and emitting signatures of potassium? The answer is one telescope does, in France, and no others. It wasn't due to potassium in the star, though, but potassium in the detector apparatus room, because people were striking matches.
4:48 PM: But. it turns out that there may be actual potassium-flare stars, since a non-smoker (haha) observed a similar signature. It is easy to fool yourself if a source you didn't account for is causing an effect, but that doesn't mean the effect you're seeing isn't actually real! For example, at the Parkes radio observatory, using the microwave at lunchtime, and opening the door, caused a brief flash of radio waves that made people think they were seeing a fast radio burst, but no, it was the microwave. Yet. fast radio bursts are real, and now we know more about them and have seen a bunch!
This artist’s impression shows the supergiant star Betelgeuse as it was revealed thanks to different state-of-the-art techniques on ESO’s Very Large Telescope (VLT), which allowed two independent teams of astronomers to obtain the sharpest ever views of the supergiant star Betelgeuse. They show that the star has a vast plume of gas almost as large as our Solar System and a gigantic bubble boiling on its surface.
ESO/L. Calçada4:51 PM: Here's a fun thing to imagine: what happens if you have a binary star system, where both are large and will go supernova? Well, one will go first, and perhaps it will produce a neutron star. Now, what happens if they spiral in, and merge? The neutron star will sink to the core, and so you get a red supergiant (eventually) with a neutron star at its core. This is what a Thorne-Zyktow object is, and it makes very explicit predictions for what you'll observe at the surface!
Here's what a Thorne-Zyktow object should do, where 1-out-of-70 observed red supergiant stars showed the spectral signature you expect.
Screenshot from Emily Levesque's Perimeter Institute lecture4:54 PM: How fun, that what's going on is a combination of nuclear physics, thermal physics, and chemistry. and that when an atomic nucleus touches the surface of the neutron star, it only stays there for about 10 milliseconds, and will produce a chemical signature we don't see anywhere else. And, lo and behold, you can find this odd, predictive chemical signature in a very small number of red supergiants, one-out-of-70, leading us to conclude that Thorne-Zyktow objects are real!
4:57 PM: I love the care that Emily is taking in calling this object a candidate, though. We have to make sure that there isn't something else mimicking the effect we expect. Even when an observation fits your theory perfectly, you need confirmation from multiple objects and multiple lines of evidence. This is the way scientists work: we have to overwhelmingly convince ourselves, or it's just likely rather than convincing.
The remnant of supernova 1987a, located in the Large Magellanic Cloud some 165,000 light years away. The fact that neutrinos arrived hours before the first light signal taught us more about the duration it takes light to propagate through the star's layers of a supernova than it did about the speed neutrinos travel at, which was indistinguishable from the speed of light. Neutrinos, light, and gravity appear to all travel at the same speed now.
Noel Carboni & the ESA/ESO/NASA Photoshop FITS Liberator5:00 PM: There's a great hope that stellar astronomers have: that someday within our lifetime, we'll have a supernova we can observe with our own naked eyes. We haven't seen one from Earth since 1604. but we could get one at any time. If you thought the eclipse was spectacular. just imagine what this would be like!
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5:02 PM: Her talk is done, and it felt like it went fast and covered a lot of ground! I'm happy that she covered so many stars and star types, but I'm a little bit sad that things didn't get weirder overall. Supernovae are great, but they're not that weird. Thorne-Zyktow objects, though. I'll give you that, those are weird!
A slew of weird objects. many of which are illustrations or simulations, but some of which are actual photos!
E. Levesque / Perimeter5:06 PM: So Emily showed these 'weird objects' and said you'd be able to identify them all. Can you? It looks like we have, counterclockwise from the upper left:
- The crab nebula (supernova remnant), which is real,
- Eta carina, which is an ejection nebula around a luminous blue variable (real),
- A binary star pair, with one of them a neutron star accreting matter (illustration),
- A gamma-ray burst (illustration),
- and a Thorne-Zyktow object (simulation).
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Not bad!
5:08 PM: And that's it! I like Emily's story of her excitement and passion, and when she knew she wanted to study the stars. Who knew from age 2? Well, Emily, born in 1984, knew: she saw Halley's comet. She was fascinated with it. and she always wanted to be an X or an astronomer. A ballerina or an astronomer. A paleontologist or an astronomer. A marine biologist or an astronomer. And now, here she is! Science activities, stories (with representation, like a Wrinkle In Time), and encouragement helped.
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Science is for everyone, and a tour of a public lecture like this is a great example of why we're glad that it is! Thanks Emily, thanks Perimeter, and thanks to you for tuning in!