A White Dwarf and a Black Hole in a Tight Orbit

Mar
13
Dr. Arash Bahramian
Dr. Arash Bahramian

We are very happy to welcome Dr. Arash Bahramian as our guest blogger. Dr. Bahramian completed his graduate studies at University of Alberta, Canada with Dr. Craig Heinke on X-ray binaries in globular clusters. After defending his PhD in 2016, he moved to Michigan State University to work with Dr. Jay Strader on study of black holes in globular clusters. He is the first author of the paper featured in our most recent press release.

Stellar mass black holes are formed by the deaths of massive stars. Like other black holes, these objects do not emit any light of their own, and astronomers try to identify them from their interactions with their environment. For example, in a close binary with another star, the black hole's strong gravity pulls material from the companion star. This material falls towards the black hole through a disk called an accretion disk. The massive release of energy due to infall of matter towards the black hole plus friction between particles in the disk, makes this disk extremely hot (about a million degrees Kelvin, roughly 200 times hotter than the surface of the Sun). This temperature is high enough to make the disk bright in X-rays, and so X-ray observatories like NASA's Chandra X-ray Observatory have been used to identify and study these systems.

Over the last few decades, dozens of stellar mass black holes (and black hole candidates) in close binaries with another star have been identified throughout our Galaxy. However, none of these black holes were found in old dense stellar clusters known as globular clusters. This was surprising at first, as we would expect a lot of black holes (maybe around 1000 of them) in these clusters, because many massive stars should have turned into black holes. Furthermore, a crowded stellar environment like a cluster makes interactions between black holes and other stars more likely. For a long time, this absence of black holes in dense stellar clusters was thought to be a result of black holes getting kicked out of the cluster, due to their strong gravity and rapid movement after interacting with other stars and other black holes in the cluster.

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From Art to Astrophysics – and Back Again

Mar
02
Melissa Weiss Walter
Melissa Weiss Walter (Photo: Brin Deuk Morris)

We are thrilled to welcome Melissa Weiss Walter as a guest blogger. As Mel describes below, she served as the graphic designer, illustrator and social media developer for Chandra's publicity and outreach efforts for many years. Recently, she has scaled back her Chandra time to focus on her personal artistic endeavors. Thankfully, she remains part of the Chandra family and continues to contribute to Chandra releases.

I have been working with the Chandra team in various capacities for close to two decades. I began creating illustrations of black holes after graduating from the University of Rhode Island. Soon after Chandra launched, I was brought on board to continue as their science illustrator and also as their graphic designer. When MySpace took off like a rocket and we realized that social media was here to stay, I also took on the role as a social media administrator.

In 2015, after working with the team full-time for fourteen years, I made the decision to take a step back. I was able to continue just with my duties in science illustration so that I could pursue a career in fine art. Though I may have discontinued my time with Chandra on a full-time basis, I took with me the inspiration of many years looking at the wonders of our Universe through Chandra's eyes.

Before making the change, I had always loved the work I did with the Chandra team. However, I was so busy creating materials that I didn't have a lot of time to reflect on the content I was using. I knew what we did was important but I never realized how influenced I was becoming by the wonders we communicated with the public on a daily basis.

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Visualizing Supernova 1987A in Three Dimensions

Feb
24
Salvatore Orlando
Salvatore Orlando

Our latest press release features work by Salvatore Orlando, an astrophysicist working at the INAF-Osservatorio Astronomico di Palermo in Italy. Salvatore and his colleagues have developed the first three-dimensional model of the famous object Supernova 1987A that links the supernova to its remnant, an accomplishment that will help scientists and the public explore this important stellar object like never before. We are very pleased to share answers that Salvatore has provided to our questions about his 3D modeling.

Salvatore graduated in physics from the University of Palermo and completed his PhD at the same university. During his PhD he spent part of this time at the Dept. of Astronomy and Astrophysics at the University of Chicago. Prior to his current position, he was a research fellow for two years at the European Space Agency (ESA), Space Science Dept. (Noordwijk, The Netherlands). His main research activity has been performed in the realm of optically thin astrophysical plasmas (more specifically solar and stellar coronae, supernova remnants) and in the field of thermal and non-thermal (synchrotron) emission processes.

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Black Holes and Vacuum Cleaners: Using Metaphors to Explain Space Images

Feb
16

Scientific imagery, especially those from space, can be both powerful and beautiful. The images created by professional and amateur astronomers alike are often striking. This gives science communicators an opportunity to use such images as an access point for the related subject matter. In other words, scientific images are a door through which we can walk towards the discoveries and insight that science can achieve.

The Aesthetics & Astronomy project (A&A) is a unique research project that aims to study exactly how people from different backgrounds and educational experiences interpret and interact with scientific imagery. Started at the Chandra X-ray Center and combining the expertise of astrophysicists, psychologists, image producers, and educators specializing in research methodology, A&A delves into how these images can be used as a vehicle for scientific information.

One question that A&A recently asked is: how effective are metaphors in communicating scientific results? To explore this question, the A&A project solicited input from nearly 2,000 participants and asked a series of questions through an online study. After presenting participants with four astronomical images — Sagittarius A*, Our Sun (solar flare), Cassiopeia A, and the Pinwheel Galaxy — they were shown three separate labels for each.

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The Poetry of a Clandestine Black Hole

Feb
15

Over several years we have hosted the results of poetry competitions organised and judged by Jonathan Taylor, a Senior Lecturer in Creative Writing at The University of Leicester in the UK. Here, Jonathan gives some details about the latest competition and discusses the link between poetry and science.

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Carnival of Space

Feb
08

It’s Carnival time, folks, so let’s get started! Here is a brief look at interesting space stories from the past week.

At Universe Today, their writers have got the Universe covered. In one post, they take a look at an intriguing new result that may help tie "Joshua's Eclipse" to the Battle of Gibeon, showing how astronomy can help make connections in other fields such as history. http://www.universetoday.com/133166/ancient-annular-dating-joshuas-eclipse/

Juno
Processed image taken on Dec. 11, 2016, at 9:27 a.m. PST (12:27 p.m. EST) by the NASA Juno spacecraft, as it performed its third close flyby of Jupiter. Credits: NASA/JPL-Caltech/SwRI/MSSS/Eric Jorgensen

In another post, they explain the most recent exciting pass of the Juno spacecraft over the cloud tops of Jupiter. NASA is also offering the public the chance to vote on what features Juno should image next. Take a look! http://www.universetoday.com/133215/juno-buzzes-jupiter-cloud-tops/

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Stellar Gluttony: Force-feeding a Massive Black Hole for over a Decade

Feb
06
Dr. Dacheng Lin
Dr. Dacheng Lin

We are pleased to welcome Dr. Dacheng Lin as our guest blogger. Dacheng is the first author of a new Nature Astronomy paper that is the subject of our latest press release. This paper describes the discovery of a super-long tidal disruption event. Dacheng is a research scientist at the University of New Hampshire. After obtaining his PhD from Massachusetts Institute of Technology, he was a postdoc at IRAP, France and then at the University of Alabama. His main research interests include X-ray binaries, intermediate-mass black holes, and tidal disruption events.

Life is full of surprises and serendipity. My first time hearing about tidal disruption events (TDEs), where tidal forces from black holes rip stars apart, was in a colloquium at MIT when I just became a graduate student. At that time, as a new astronomer, I was hesitant to accept this "crazy" concept.

My involvement with TDE research began when I was a postdoc at IRAP, France. At that time, I took a long, systematic look at thousands of sources detected by a European Space Agency X-ray observatory called XMM-Newton. From that project I learned that most X-ray sources are active galactic nuclei (AGNs), which are supermassive black holes (SMBHs) at the center of galaxies that pull in – that is accrete – surrounding gas and emit copious amounts of radiation, including X-rays. Radiation from AGNs do not vary a lot because the gas surrounding them extends over a large scale and can last for tens of thousands of years.

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Chandra Images Show That Geometry Solves a Pulsar Puzzle

Jan
18

Geminga and B0355+54

NASA'S Chandra X-ray Observatory has taken deep exposures of two nearby energetic pulsars flying through the Milky Way galaxy. The shape of their X-ray emission suggests there is a geometrical explanation for puzzling differences in behavior shown by some pulsars.

Pulsars - rapidly rotating, highly magnetized, neutron stars born in supernova explosions triggered by the collapse of massive stars- were discovered 50 years ago via their pulsed, highly regular, radio emission. Pulsars produce a lighthouse-like beam of radiation that astronomers detect as pulses as the pulsar's rotation sweeps the beam across the sky.

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X-rays From the Young Monsters: Studying Supermassive Black Holes in the Early Universe

Jan
04
Fabio Vito
Fabio Vito

We are pleased to welcome Fabio Vito as our guest blogger. Fabio and his colleagues led some of the latest work involving the Chandra Deep Field-South that were presented at the 229th meeting of the American Astronomical Society in January 2017. He obtained a Ph.D. degree in Astrophysics and Cosmology from the University of Bologna (Italy) in 2014. During his studies he collaborated with researchers from the Astronomical Observatory of Bologna and also spent a 6-months period at the University of Cambridge (UK). After one year in a postdoctoral position in Bologna, he moved to his current position as a postdoctoral researcher at the Pennsylvania State University. Fabio's work is mainly focused on the growth and evolution of supermassive black holes in the early Universe, exploiting some of the deepest X-ray data available.

Black holes are among the most fascinating objects in the Universe. Probably most people have at least heard about them, maybe reading about some pseudo-scientific speculations like wormholes, time travelling, etc. Or perhaps they have watched movies such as the famous 2014 movie "Interstellar", or even by listening to music, such as the "Supermassive Black Hole" song by the British band Muse.

However, despite their popularity, our knowledge of these monsters of the Universe is limited. We know that "normal" black holes (although nothing is normal about black holes), which have masses of a few to tens of times the Sun's mass, are formed when big stars die and explode as supernovas. However, there is more than just one type of black hole. At the centers of most galaxies, there is a "monster among the monsters." This is what astronomers call a supermassive black hole (SMBH), and they can weigh from millions to billions of solar masses. Despite the fact that almost all of the normal-sized galaxies in the Universe host a SMBH in their centers (even our Milky Way!), astronomers do not know when and how they formed.

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The Discovery of Particle Re-acceleration in a Galaxy Cluster Collision

Jan
04
Felipe Andrade-Santos and Reinout van Weeren
Felipe Andrade-Santos and Reinout van Weeren

For this guest blog post, we are lucky to have not one, but two, contributors. Reinout van Weeren obtained his PhD from Leiden University, The Netherlands, before moving to the Harvard-Smithsonian Center of Astrophysics as an Einstein Postdoctoral Research Fellow. He is currently a Clay Fellow at the same place. He works on merging galaxy clusters, focusing on combined radio and X-ray observations. Felipe Andrade-Santos obtained his PhD from the Universidade de São Paulo, Brazil, before becoming a postdoctoral research fellow at the Harvard-Smithsonian Center of Astrophysics. He works on X-ray observations of galaxy clusters and galaxy cluster samples. Reinout and Felipe recently presented their study on the merging galaxy cluster system Abell 3411 and 3412 at the 229th meeting of the American Astronomical Society meeting in January 2017.

Galaxy clusters are the most massive objects in the Universe bound together by gravity and contain up to a few thousand galaxies. They are also permeated by very thin 100-million-degree gas that is held together by the cluster's strong gravitational pull. This hot gas can be imaged with X-ray satellites such as NASA's Chandra X-ray Observatory. Galaxy clusters form by mergers of smaller clusters and galaxy groups. During a merger event, which typically lasts for about a billion years, the galaxies mostly fly past each other without strongly interacting. In contrast, the diffuse gas in the merging clusters collides, creating giant shock waves, which are cosmic versions of sonic booms generated by supersonic aircraft. Cluster mergers have been of great interest to astronomers and us because of the extreme physical processes that take place during such events.

Radio telescopes have shown that large regions of merging galaxy clusters glow at radio wavelengths. The radio emission is produced by tiny particles, called electrons, which spiral around magnetic field lines and have energies that are a million times higher than the particles making up the hot cluster gas. Astronomers have long been puzzled by how these energetic electrons are produced. One idea is that the energetic particles are accelerated to these extreme energies by shocks created when clusters collide and merge.

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