October 29, 2012 at 17:14 pm | 1 Comment
This is Our Home Galaxy, and a Couple of Neighbors
When you look out at the night sky, you’re looking at our ancient home. Yes, Earth is our current home. But, in the grand scheme of things, the galaxy — and all the elements that make it are also our home. The elements that make up our bodies, our planets, and our star all were either created in the Big Bang (hydrogen, for example), or inside other stars (carbon, oxygen, nitrogen, etc.). Multiple generations of stars have lived and died in the galaxy, and we are the resulting “star stuff”.
But, there’s more than star stuff out there. There are mysterious things that may tell astronomers more about types of matter in the cosmos and distribution of that matter throughout the universe.
Astronomers have been studying one of those two irregular-looking clouds of stars that appear just below our galaxy in this image to understand a category of objects called MACHO (Massive Compact Halo Objects). These were thought to be things about the mass of a star that were so faint they couldn’t be easily detected. Surveys of this region of our galactic neighborhood have been underway to see if MACHOs could be part of that mysterious collection of “stuff” called “dark matter” that seems to be an incredibly important part of the universe.
In order for MACHOs to make up dark matter, they must be very faint. To even decide if they’re “there”, astronomers looked for a phenomenon known as microlensing. During a microlensing event, a nearby object passes in front of a more distant star. The gravity of the closer object bends light from the star like a lens, magnifying it and causing it to brighten. If a MACHO does this, then they’d know a little bit more about the object.
By studying the LMC, astronomers hoped to see MACHOs within the Milky Way lensing distant LMC stars. The number of microlensing events observed by various teams was smaller than needed to account for dark matter, but much higher than expected from the known population of stars in the Milky Way. This left the origin of the observed events a puzzle and the existence of MACHOs as exotic objects a possibility.
Instead of MACHOs, a trail of stars removed from the SMC could well be responsible for the microlensing events. How do astronomers know this? They’ve done computer simulations showing that the most likely explanation for the observed microlensing events was an unseen population of stars removed by the LMC from its companion, the SMC. Foreground stars in the LMC are gravitationally lensing the trail of removed stars located behind the LMC from our point of view.
Although the evidence for the trail of lensed stars is persuasive, they haven’t been directly observed yet. That will take time, since these could be faint. A number of teams are searching for the signatures of these stars within a bridge of gas that connects the Magellanic Clouds. The computer models used to simulate the trail will point the way for astronomers to find the other “stuff” that makes up the galaxies… and intergalactic space.
October 22, 2012 at 20:36 pm | Leave a Comment
G2 Is Entering the Galactic House
The heart of our Milky Way Galaxy is home to a black hole named Sagittarius A* (known as Sag A* for short). It contains the equivalent of three to four million times the mass of the Sun, and as black holes, it’s kind of a quiet, friendly one. By that, I mean that it’s not constantly gulping down massive amounts of material as some other galaxies’ black holes do. Sure, it does eat, but it seems to do so only sporadically.
Astronomers and lab physicists at the Lawrence Livermore Labs have created a supercomputer simulation showing a gas cloud called G2 which is on its way to being Sag A*’s latest snack.
They came up with six simulations showing how the event might unfold as the cloud approaches the black hole. The cloud’s makeup is still not well-understood and astronomers are still trying to figure out where it came from in the first place. It first showed up in 2002, and observers rushed to chart its size and other characteristics. The cloud appears to have a fair amount of dust that is quite warm — 500 degrees Kelvin, which is about twice as hot as Earth’s surface. The gas entrained in the cloud is superheated hydrogen and is about twice as hot as the surface of the Sun.
This cloud could be a burp of gas from an old star that was starting to lose some of its mass. Or, as some astronomers have suggested, it might have been material that didn’t quite form a planet. And, now it’s heading toward the region of the black hole, poised for a close brush with the gravity well of the black hole sometime in September 2013. As it gets nearer, the cloud will get heated to incredibly high temperatures which will make it easy to spot using radio and x-ray telescopes on Earth.
It’s likely that not all of the cloud will get sucked into the realm of the black hole. A great deal of it may pass well outside of the “point of no return” near the black hole. But, it will get shredded apart by the close encounter with the black hole’s incredibly strong gravitational pull.
Astronomers will be able to watch the black hole dally with the cloud (like a cat dallies with a mouse) for a few years. The closest approach of the cloud will take a few months, and they should be able to track as the cloud is affected by its encounter and breaks apart.
October 21, 2012 at 21:38 pm | Leave a Comment
Be Realistic about Observing
One of the truisms in amateur astronomy is that the minute something exciting is predicted to occur in the sky, the sky immediately clouds up. This is true especially if there’s an especially juicy coronal mass ejection inciting some space weather in Earth’s close neighborhood. Or, perhaps an occultation of a star by the Moon. As soon as the news gets out, the clouds start to gather.
This happened to me on October 8th, when the space weather forecast showed a good chance of seeing aurorae even at the mid-latitudes. I mentioned this as part of a talk I gave onboard a cruise ship that day (I do astronomy enrichment presentations for the Smithsonian and Celebrity Cruise Lines) and of course it clouded up that night. But, we persevered, and eventually a sucker hole did open in the clouds that revealed some of the sky, and we saw a gorgeous greenish display to the north, complete with spiky formations that came and went.
Another case in point has been the media hype for the Orionid Meteor shower that was supposed to deliver dozens or more meteors per hour. The news media picked up on this right away, and I saw at least one headline about “spotting a stunning meteor shower” from a news organization that used to have a qualified science writer on its staff but now just rewrites from a press release, spices it up, and then publishes hypey stuff that they think will grab people’s attention. (Yes, CNN, I’m talking about you…)
The press release I got from a reputable observatory mentioned that it might be possible to see up t0 25 meteors per hour. No promises, just a possibility. No flashy graphics about “dazzling” sights… And, reports I’ve seen from actual observers indicate that the counts have been a bit less than normal.
This is the sort of thing that really ought to give the media a bad name for over-hyping. A competent science writer would have been able express the story much more clearly for readers/viewers and given a more realistic view of what the shower might look like.
The reality of observational astronomy is that sometimes something can be quite spectacular, and sometimes it just isn’t. Astronomers’ models can only go so far in predicting how good a meteor shower, for example, will look. There are a lot of other factors that influence your observational experience… including clouds.
The best thing to do is get out there and observe… there are some gorgeous skies coming our way over the next few months, so be ready for them! Cherish each meteor, search out the planets, check out the nebulae, and never stop looking for the wonders to be seen in the night-time sky!
October 3, 2012 at 16:53 pm | Leave a Comment
Herschel Discovers Cometary Crystals around Beta Pictoris
We all know about comets in our own solar system. They’re conglomerates of ices mixed with dust and rock. As they get close to the Sun their gases sublimate, the dust is freed and that action creates dust and plasma tails streaming out behind the comet. Astronomers see comets as repositories of information (in the form of those ices and dust particles) about conditions in the early solar system, since those materials have survived until this time. In particular, comets often contain materials that formed close to the Sun in the early history of the solar system, but then were somehow transported out to colder regions where comets seem to thrive.
So, it’s rather cool that astronomers have now found cometary particles in another solar system, the young star Beta Pictoris. The European Space Agency’s Herschel space telescope detected pristine materials in the dust disk surrounding this star. Those materials match the makeup of comets in our own solar system.
Beta Pictoris hosts a gas giant planet, in addition to a dusty debris disk that will likely spawn the formation of some icy bodies similar to the worldlets that astronomers are finding in our own Kuiper Belt.
So, what’s the material made of that Herschel found? First, the mineral olivine is present in the disk around Beta Pic. Olivine forms in protoplanetary disk material close to newly formed stars. In our solar system we find it in asteroids and comets, and of course it’s found on Earth, too.
The data collected by the Herschel telescope allowed astronomers to calculate that the olivine crystals in the Beta Pic disk make up about 4% of the total mass of the dust found in a region that lies between 15 to 45 astronomical units from the star. In our solar system, that extends from well beyond the orbit of Saturn out beyond the inner limit of the Kuiper Belt. The 4% number is quite similar to such solar system comets as 17P/Holmes and 73P Schwassmann-Wachmann 3.
Astronomers concluded that the olivine was originally bound up inside comets and released into space by collisions between the icy objects. And, since since olivine can only crystallize at a distance of not more than 10 astronomical units of the central star, finding it in a cold debris disc means that it must have been transported from the inner region of the system out to colder areas. A process called “radial mixing” could help push materials out away from the central star, and that could explain how the olivine crystals made it to the deep freeze of the Beta Pic system. Want to read more about this find? Check out ESA’s Herschel Web page for the full story.
Get Your Stargazing On for October!
This month’s edition of “Our Night Sky”, the star gazing video I produce for AstroCast.tv is now up for your viewing pleasure! Check it out!
This blog a wholly pwnd subsidiary of Carolyn Collins Petersen, a.k.a. TheSpacewriter.
Copyright 2013, Carolyn Collins Petersen
Image of Horsehead Nebula: T.A.Rector (NOAO/AURA/NSF) and Hubble Heritage Team (STScI/AURA/NASA)
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