[X-ray emission from two nearby millisecond pulsars final technical report]. by Stephen Erik Thorsett

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Published by California Institute of Technology, National Aeronautics and Space Administration, National Technical Information Service, distributor in Pasadena, CA, [Washington, DC, Springfield, Va .

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Series[NASA contractor report] -- NASA CR-196142.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL17001668M
OCLC/WorldCa32265292

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Get this from a library. [X-ray emission from two nearby millisecond pulsars: final technical report]. [Stephen Erik Thorsett; United States. National Aeronautics and Space Administration.]. Characteristics. An X-ray pulsar consists of a magnetized neutron star in orbit with a normal stellar companion and is a type of binary star magnetic-field strength at the surface of the neutron star is typically about 10 8 Tesla, over a trillion times stronger than the strength of the magnetic field measured at the surface of the Earth (60 μT).

Millisecond pulsars are ones that spin particularly rapidly, hundreds of times per second. Astronomers probe the emission from a nearby pulsar wind nebula.

Strong X-ray pulsations detected. X-RAY EMISSION FROM THE NEARBY PSR B+16 AND OTHER OLD PULSARS O. Kargaltsev, G.

Pavlov, and G. Garmire Pennsylvania State University, Davey Lab, University Park, PA ; [email protected], [email protected], [email protected] Received June 13; accepted September 2 ABSTRACT. Ordinary radio pulsars 1 are neutron stars with magnetic fields of ∼ 10 12 gauss and spin periods in the range to 3 seconds.

In contrast, millisecond radio pulsars 2 have much weaker fields. High-Energy Emission From Millisecond Pulsars Alice K. Harding', Vladimir V.

Usov2 & Alex G. Mu~limov'~~ ABSTRACT The X-ray and yray spectrum of rotation-powered millisecond pulsars is in- vestigated in a model for acceleration and pair cascades on open field lines above the polar caps.

Although these pulsars have low surface magnetic fields, their. or inverse Compton emission, as seen in wind nebulae around young pulsars. In either case, the x-ray emission requires a population of relativistic particles in the pulsar wind.

Thus, the detection of a distinct x-ray tail provides direct evidencethat millisecond pulsars lose their rotational energy through relativistic winds. A millisecond pulsar (MSP) is a pulsar with a rotational period smaller than about 40 econd pulsars have been detected in radio, X-ray, and gamma ray parts of the electromagnetic leading theory for the origin of millisecond pulsars [X-ray emission from two nearby millisecond pulsars book that they are old, rapidly rotating neutron stars that have been spun up or "recycled" through accretion of.

The radio emission from pulsars F Graham-Smith Reports on Progress in Physics 66 IOPscience. On the Origin of X-Ray Emission from Millisecond Pulsars in 47 Tucanae K. Cheng and Ronald E. Taam The Astrophysical Journal IOPscience.

Chandra Study of a Complete Sample of Millisecond Pulsars in 47 Tucanae and NGC Radio emission from two anomalous X-ray pulsars Article (PDF Available) in Astronomy Reports 49(3) January with 31 Reads How we measure 'reads'.

Millisecond pulsars are the product of a two stage process: The X-ray emission from a neutron star in a binary system comes mainly from. Approximately uniformly across the entire sky. Gamma ray bursts are observed to occur. More than 25x that of the shn.

The idea of neutron stars can be traced back to the early s, when Subrahmanyan Chandrasekhar discovered that there is no way for a collapsed stellar core with a mass more than times the solar mass, M, to hold itself up against gravity once its nuclear fuel is exhausted.

This implies that a star left with M › M (the Chandrasekhar limit) would keep collapsing and Cited by: X-ray bursters occur in binary star systems.

The two types of stars that must be present to make up such an object are You would expect millisecond pulsars to be. ( c) fires a laser beam directly ahead of itself.

An astronaut watching this from a nearby stationary asteroid see the laser beam traveling at x the speed of light (1. @article{osti_, title = {A NuSTAR OBSERVATION OF THE GAMMA-RAY-EMITTING X-RAY BINARY AND TRANSITIONAL MILLISECOND PULSAR CANDIDATE 1RXS J–}, author = {Bogdanov, Slavko}, abstractNote = {I present a 40 ks Nuclear Spectroscopic Telescope Array observation of the recently identified low-luminosity X-ray Cited by: 6.

Transitional Millisecond Pulsars • Lack of radio pulsar emission when accreting –enshrouding or quenching due to accretion. • Flat-spectrum radio continuum emission –jet-like outflow. • X-ray mode switching –emptying and refilling of inner accretion. Observations with the Chandra X-Ray Observatory have given astronomers some clues about what causes millisecond pulsars - extremely dense stars which can spin many times a second.

Several of these. Abstract: X-ray emission is a common feature of all varieties of isolated neutron stars (INS) and, thanks to the advent of sensitive instruments with good spectroscopic, timing, and imaging capabilities, X-ray observations have become an essential tool in the study of these objects.

Non-thermal X-rays from young, energetic radio pulsars have been detected since the Cited by:   The pulsar in J falls into the category of accreting millisecond X-ray pulsars (AMXP), which are pulsars that emit X-rays and have a rotational period that doesn’t exceed 10 milliseconds.

J’s pulsar spins about 9, times per minute and shoots out X-rays with a frequency of times per : Alexandra Lozovschi. The peculiar cosmic object known as 47 Tuc W (denoted by arrow in the X-ray image) is a double star system consisting of a normal star and a neutron star that makes a complete rotation every Observations of millisecond X-ray pulsars Rudy Wijnands The other four accreting millisecond pulsars were discovered within the last two years and only limited results have been published so far.

A more extended review can be found at A model of the X-ray and optical emission from the system using an X. We have detected pulsed X-ray emission from the fastest millisecond pulsar known, PSR B+21 (P = ms), with ASCA. The pulsar is detected as. A millisecond pulsar is a type of radio or X-ray pulsar that has a rotation period measured in a small number of milliseconds, usually below 30 ms.

History The first millisecond pulsar was the celebrated ms pulsar PSR B+21, which, for over 20 years was the fastest pulsar known. This pulsar had a very small magnetic field strength (~10 Gauss) and a rotation period.

With significantly higher sensitivities compared with previous X-ray satellites they allowed for the first time to detect X-ray emission from objects as faint as millisecond (ms) pulsars.

In this paper we summarize the current observational status and discuss the empirical constraints on the pulsars’ X-ray emission by: 1.

High-Energy Properties of Pulsed Emission from Millisecond Pulsars: Authors: and the X-rays are produced by the backflow current of the outer gap and consist of one power-law and two thermal components. These X-rays collide with high-energy photons inside the outer gap to sustain the outer gap, and then high-energy γ-rays are produced in.

The Huntsman’s Future. A second system fitting the huntsman classification was recently described by the same team responsible for the J report.

Ideally, it will eventually be possible to obtain X-ray observations of the entire binary orbit to determine whether these systems indeed show significant periodic X-ray emission consistent with the proposed. X-Ray Properties of Rotation-Driven Pulsars The middle aged pulsars (i.e.

the cooling neutron stars) show emission properties which are found to be described by a dichotomy (i.e. two spectral components, soft component is of thermal origin, hard component of non-thermal origin, transition point at about keV).Cited by: 2.

An earlier study of another system with the GBT detected the first evidence of an accretion disk around a neutron star, which helped establish the link between low.

THERMAL X-RAYS FROM MILLISECOND PULSARS: CONSTRAINING THE FUNDAMENTAL PROPERTIES OF NEUTRON STARS accepted August 1 ABSTRACT We model the X-ray properties of millisecond pulsars (MSPs) by considering hot-spot emission from a weakly The X-ray emission from these pulsars is consistent with the presence of an atmosphere and a.

Abstract Ordinary radio pulsars are neutron stars with magnetic fields of ~10 12 gauss and spin periods in the range to 3 seconds. In contrast, millisecond radio pulsars have much weaker fields (~10 9 gauss) and faster, millisecond spin rates.

For both types of pulsar, the energy driving the radio pulsations is thought to be derived from the rotation of the neutron star. T1 - X-ray and gamma-ray emissions from rotation powered millisecond pulsars. AU - Takata, J. AU - Cheng, K. AU - Taam, Ronald E. PY - /1/ Y1 - /1/ N2 - The Fermi Large Area Telescope has revealed that rotation powered millisecond pulsars (MSPs) are a major contributor to the Galactic γ-ray source by: strongly a ect X-ray emission from near the star in two ways.

(1) The pairs are a source of synchrotron emission immediately following their creation in regions where B˘ G. This emission, in the photon energy range keV ˘. (tens of billions of years) than the normal pulsars.

As a result, the millisecond pulsars are exceptionally stable clocks, whose stability rivals modern atomic clocks (see Fig. Why Observe Pulsars in the X-ray Band. Nearly all pulsars (more than are now known) are discovered and studied in the radio band, using ground-based telescopes.

Pulsars are magnetized neutron stars that appear to emit periodic short pulses of radio radiation with periods between ms and s. The radical proposal that neutron stars even exist was made with trepidation by Baade & Zwicky in []: “With all reserve we advance the view that a supernova represents the transition of an ordinary star into a new form of star, the neutron.

X-ray pulsars are binary systems in which the X-ray emission is powered by the release of gravitational potential energy as material is accreted from a massive companion. But until recently, the energy source for anomalous X-ray pulsars (AXP) was a mystery – hence the term anomalous in the name.

X-ray binaries are a class of binary stars that are luminous in X-rays are produced by matter falling from one component, called the donor (usually a relatively normal star), to the other component, called the accretor, which is very compact: a neutron star or black infalling matter releases gravitational potential energy, up to several tenths of its rest mass, as X-rays.

IN the binary millisecond pulsar system PSR + 20 (ref. 1), a wind from the pulsar is ablating a low-mass ( solar mass) companion and also inflating a local nebula2 confined by the ram. We report on intermittent X-ray pulsations with a frequency of Hz from the neutron-star X-ray binary SAX J in the globular cluster NGC A CfA study of the bright radio jet galaxy Pictoris suggests that bright X-ray emission from the jets is produced by rapidly moving charged particles in magnetic fields.

CfA astronomers have identified white dwarf companions of two more millisecond pulsars in the spectacular globular cluster 47 Tucanae.

There are two groups of binary pulsars, the PSR +group, which descended from massive X-ray binaries, and the PSR +group, which descended from fairly wide low-mass X-ray binaries. At least several neutron stars in the second group have formed by the accretion-induced collapse of a massive white by: 3.

A. Patruno & A. Watts “Accreting Millisecond X-Ray Pulsars” Public List of LAT-Detected Gamma-Ray Pulsars M. Roberts “Surrounded by Spiders” Source Type Notation: MSP = millisecond pulsar in the field MSP-GC = millisecond pulsar in globular cluster RB-F = Redback in the field RB-GC = Redback in globular cluster.

Using NASA's Rossi X-ray Timing Explorer, scientists have discovered a limit to how fast a pulsar can spin without destroying itself. Gravitational radiation, ripples in the fabric of space predicted by Albert Einstein, may serve as a cosmic traffic enforcer, protecting reckless pulsars from spinning too fast and blowing apart, according to a report published in the July 3 issue of Nature.

X-ray Pulsar Scientists analyzing the first data from the Neutron star Interior Composition Explorer (NICER) mission have found two .Millisecond pulsars binaries are gamma-ray emitters. • 2. Millisecond pulsars binaries may transit between different states (radio pulsar state, sub-luminous state, accreting state).

• 3. The gamma-ray emitting processes are different in different states/different millisecond pulsars • 4.

Only three transitional millisecond pulsars.

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