{"id":774838,"date":"2023-11-30T18:52:50","date_gmt":"2023-11-30T23:52:50","guid":{"rendered":"http:\/\/spaceweekly.com\/?p=774838"},"modified":"2023-11-30T18:52:50","modified_gmt":"2023-11-30T23:52:50","slug":"spider-pulsars-are-tearing-apart-stars-in-the-omega-cluster","status":"publish","type":"post","link":"https:\/\/spaceweekly.com\/?p=774838","title":{"rendered":"Spider Pulsars are Tearing Apart Stars in the Omega Cluster"},"content":{"rendered":"


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Pulsars are extreme objects. They\u2019re what\u2019s left over when a massive star collapses on itself and explodes as a supernova. This creates a neutron star. Neutron stars spin, and some of them emit radiation. When they emit radiation from their poles that we can see, we call them pulsars. <\/p>\n

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In the last decade or so, astrophysicists have discovered many more millisecond pulsars, ones that rotate very rapidly. Not only is the number of known pulsars increasing, but researchers have also identified pulsar sub-types that have companions. These are called spider pulsars, and their companions face great peril. New research sheds light on how spider pulsars in Omega Centauri are tearing their companions to pieces with their powerful outflows.<\/p>\n

The first spider pulsar ever discovered is PSR B1957+20, more widely known as the Black Widow Pulsar. It has a companion that\u2019s either a brown dwarf or a super Jupiter. High-energy outflows from the Black Widow are destroying its companion. All pulsars that destroy their companions are known as spider pulsars, but there are two further sub-types of spider pulsars: redback pulsars and black widow pulsars.<\/p>\n

Artist\u2019s impression of the pulsar PSR B1957+20 (seen in the background) through the cloud of gas enveloping its brown dwarf star companion. Credit: Dr. Mark A. Garlick; Dunlap Institute for Astronomy & Astrophysics, University of Toronto<\/figcaption><\/figure>\n

Researchers working with the Chandra Space Telescope have examined Omega Centauri to learn more about how spider pulsars destroy their binary companions. Their work will be published in the Monthly Notices of the Royal Astronomical Society. The title is \u201cA Chandra X-ray study of millisecond pulsars in the globular cluster Omega Centauri: a correlation between spider pulsar companion mass and X-ray luminosity.\u201d The authors are Jiaqi Zhao and Craig O. Heinke, both from the Physics Department at the University of Alberta, Edmonton, Canada.<\/p>\n

Omega Centauri is the largest globular cluster (GC) that we know of in the Milky Way. It\u2019s almost 16,000 light-years away and contains about 10 million stars. Some of those stars are spider pulsars, a class of millisecond pulsars with companions. <\/p>\n

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Visualization of a fast-rotating pulsar. Credit: NASA\u2019s Goddard Space Flight Center Conceptual Image Lab<\/figcaption><\/figure>\n

Spider pulsars are terribly destructive neighbours. Their energetic winds methodically strip away their companions\u2019 outer layers. To understand more about this phenomenon, the pair of researchers examined Chandra data from Omega Centauri, home to 18 recently discovered spider pulsars. <\/p>\n

\u201cMillisecond pulsars (MSPs) are faint X-ray sources commonly observed in Galactic globular clusters (GCs),\u201d the researchers write. \u201cIn this work, we investigate 18 MSPs newly found in the GC Omega Centauri and search for their X-ray counterparts using Chandra observations.\u201d <\/p>\n

Out of the 18 millisecond pulsars, 11 of them emit x-rays that Chandra can see. Five of them are spider pulsars near Omega Centauri\u2019s center. They combined these with Chandra\u2019s observations of 26 spider pulsars in 12 other globular clusters. Using this data, the pair of researchers examined empirical correlations between X-ray luminosities and the minimum masses of their companions. <\/p>\n

\"This
This image shows Omega Centauri\u2019s central region in both optical light and X-rays, with some of the millisecond pulsars labelled. Image Credit: X-ray: NASA\/CXC\/SAO; Optical: NASA\/ESA\/STScI\/AURA; Image Processing: NASA\/CXC\/SAO\/N. Wolk<\/figcaption><\/figure>\n

There are two classes of spider pulsars, and they\u2019re based on their companions\u2019 masses. Redback spider pulsars have companions between one-tenth and one-half of a solar mass, while black widow class pulsars have companions with less than 5% of the Sun\u2019s mass. <\/p>\n

The researchers found that redback spider pulsars are brighter in X-rays than black widow pulsars. This is in line with previous research. <\/p>\n

But this is the first time that research has shown a correlation between X-ray luminosity and companion mass. We can see in the data how redback spiders with more luminous X-rays have more massive companions. That might seem counter-intuitive on the surface. What\u2019s behind it? <\/p>\n

\"This
This figure from the research shows the X-ray luminosity of the spider pulsars on the y-axis and the minimum masses of their companion stars on the x-axis (logarithmic). There\u2019s a clear correlation between redblack spider pulsars, shown in red circles, and black widow pulsars, shown in black, and their companions\u2019 masses. (M14-A and M30-A are outliers.) Image Credit: Zhao and Heinke, 2023.<\/figcaption><\/figure>\n

Spider pulsars create X-rays when particles in their stellar winds strike the winds coming from their companions and produce shock waves. The more massive its companion is, the stronger the companion\u2019s winds. That means the colliding winds produce more luminous X-rays.<\/p>\n

\u201cTherefore, our findings indicate that as the companion mass increases, the X-ray luminosity of the
spider pulsar tends to increase as well,\u201d the authors write in their paper. \u201cIt likely suggests that a more
massive companion can produce stronger winds and thus generate stronger intra-binary shocks with relativistic pulsar winds, leading to higher X-ray luminosities as observed.\u201d<\/p>\n

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