Possible Conversion of Rotational Energy of the Neutron Star in the Crab Nebula Into Energy of Relativistic Electrons

1969 ◽  
Vol 155 ◽  
pp. L107 ◽  
Author(s):  
A. Finzi ◽  
R. A. Wolf
Keyword(s):  
Neutron Star ◽  
Crab Nebula ◽  
Rotational Energy ◽  
Relativistic Electrons ◽  
The Crab Nebula

scholarly journals Physical Processes and Parameters in the Magnetosphere of NP 0532

1971 ◽  
Vol 46 ◽  
pp. 394-406
Author(s):  
F. Pacini
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
General Relation ◽  
Energy Generation ◽  
Main Pulse ◽  
Physical Processes ◽  
X Ray ◽  
The Crab Nebula

The Crab Nebula pulsar conforms to the model of a rotating magnetised neutron star in the rate of energy generation and the exponent of the rotation law.It is suggested that the main pulse is due to electrons and the precursor to protons. Both must radiate in coherent bunches. Optical and X-ray radiation is by the synchrotron process.The wisps observed in the Nebula may represent the release of an instability storing about 1043 erg and 1047–48 particles.Finally, some considerations are made about the general relation between supernova remnants and rotating neutron stars.

scholarly journals On the Nature of the Emission of the Crab Nebula

1958 ◽  
Vol 8 ◽  
pp. 1047-1047
Author(s):  
I. S. Shklovsky
Keyword(s):  
Field Strength ◽  
Magnetic Energy ◽  
Crab Nebula ◽  
Central Star ◽  
Emission Sources ◽  
Relativistic Electrons ◽  
Internal Motions ◽  
The Crab Nebula ◽  
Lines Of Force

The emission of the Crab Nebula is perhaps connected with the internal motions of the gas. As shown by the observations, the power of the emission sources differs by some hundred times in different points of the amorphous mass (“wisps” and other details). Oort and Walraven believe the “wisps” to be condensations of relativistic electrons ejected from the central star. However, there are some other variable details elsewhere in the nebula (as described by Lampland, and Oort and Walraven).Oort and Walraven's hypothesis met some important difficulties: (a) the direction of the magnetic lines in this region of the nebula is perpendicular to the wisp's velocity; (b) the dimension of the wisp is about three light months, while it appears during a month and faster, so that the relativistic electrons moving along the lines of force have no time to spread along the wisp; and (c) if the strength is not changing, the energy of the relativistic electrons in the wisp must be some hundred times greater than the density of the magnetic energy, consequently the field strength must grow in the wisp to keep the electrons in the volume.

scholarly journals Transfer of Energy to the Crab Nebula Following the Spin-Up of the Pulsar

1971 ◽  
Vol 46 ◽  
pp. 296-307 ◽  
Author(s):  
D. B. Melrose
Keyword(s):  
Energy Flux ◽  
Central Region ◽  
Crab Nebula ◽  
Point Of View ◽  
Relativistic Electrons ◽  
Synchrotron Emission ◽  
X Ray ◽  
Enhanced Activity ◽  
The Crab Nebula

Observed enhanced activity in the central region of the Crab Nebula following the spin-up of the pulsar is discussed from the point of view of the transfer of energy to relativistic electrons. It is argued that a rapid deposition of energy associated with the spin-up of the pulsar causes a radial energy flux which becomes a flux in hydromagnetic activity at about the regions where enhanced synchrotron emission is observed. It is shown that such hydromagnetic activity is rapidly damped by the relativistic electrons with energy being transferred to the relativistic electrons. This acceleration can account for the short synchrotron halflifetimes observed. The model predicts highly enhanced X-ray emission from the central region of the Nebula following a spin-up.

scholarly journals Timing of Optical Pulses from the Crab Nebula Pulsar

1971 ◽  
Vol 46 ◽  
pp. 119-124
Author(s):  
P. E. Boynton ◽  
E. J. Groth ◽  
R. B. Partridge ◽  
David T. Wilkinson
Keyword(s):  
Neutron Star ◽  
Crab Nebula ◽  
Physical Models ◽  
Quiet Period ◽  
Eccentric Orbit ◽  
Optical Pulses ◽  
Neutron Star Crust ◽  
Alternate Explanation ◽  
Speed Up ◽  
The Crab Nebula

Timing the arrival of optical pulses from NP 0532 is a potentially important tool for studying the physics of this fascinating object. However, there are some difficulties in interpreting the data in terms of physical models. Some progress has been made on understanding the largest effect – the pulsar braking mechanism. The glitch of late September, 1969 can be interpreted as the speed-up, and subsequent relaxation, of the rotation of a neutron star crust. An alternate explanation is that of a planet in an eccentric orbit. Both models fit the rather meager data near the event. A small sinusoidal effect is indicated in a relatively quiet period of the data.

scholarly journals The Galactic Sources G5.4-1.2 and G5.27-0.90

1987 ◽  
Vol 125 ◽  
pp. 129-129
Author(s):  
J.L. Caswell ◽  
M.J. Kesteven ◽  
R.F. Haynes ◽  
D.K. Milne ◽  
M.M. Komesaroff ◽  
...  
Keyword(s):  
Neutron Star ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Stellar Core ◽  
Galactic Sources ◽  
The Crab Nebula

Long after a supernova event, the stellar core (neutron star) may continue to excite an extended remnant of ejecta surrounding it, as in the case of the Crab nebula. In contrast, the more common shell supernova remnants (SNRs) appear unaffected by any embedded neutron star.

scholarly journals Superfluidity in Neutron Stars

1974 ◽  
Vol 53 ◽  
pp. 151-165
Author(s):  
George Greenstein
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Crab Nebula ◽  
Crab Pulsar ◽  
X Ray ◽  
Effects Of Rotation ◽  
The Crab Nebula

We present a short Cook's tour of the possible effects of rotation coupled with superfluid properties of neutron star interiors. A suggestion is made to take advantage of forthcoming lunar occultations of the Crab Nebula in order to search for blackbody X-ray emission from the Crab pulsar.

scholarly journals Relationship Between Pulsar and Nebula

1971 ◽  
Vol 46 ◽  
pp. 389-391
Author(s):  
L. Woltjer
Keyword(s):  
Magnetic Field ◽  
Energy Density ◽  
Energy Supply ◽  
Crab Nebula ◽  
Supernova Explosion ◽  
Relativistic Electrons ◽  
The Crab Nebula ◽  
The Magnetic Field

The magnetic field and the relativistic electrons in the Crab Nebula cannot have originated at the time of the supernova explosion. The energy density in the magnetic field is so large that it must have been generated using the energy supply in the pulsar. The energies of the electrons are so high, and their lifetimes correspondingly are so short, that they must have been accelerated, again using the pulsar energy. The efficiency of these processes must be high, but there is an adequate energy supply.

scholarly journals The Nature of the Energy Source in Radio Galaxies and Active Galactic Nuclei

1982 ◽  
Vol 97 ◽  
pp. 247-253
Author(s):  
F. Pacini ◽  
M. Salvati
Keyword(s):  
Energy Source ◽  
Active Galactic Nuclei ◽  
Crab Nebula ◽  
A Priori ◽  
Galactic Nuclei ◽  
High Energy ◽  
Galactic Cosmic Rays ◽  
Relativistic Electrons ◽  
Probable Presence ◽  
The Crab Nebula

For more than 20 years it has been known that extragalactic radio sources contain up to 1060–1062 ergs in the form of relativistic electrons and magnetic fields. One arrives at these figures if one assumes that the radio emission is due to the synchrotron process and the source contains an equal amount of energy in electrons and fields (Burbidge 1956). Any deviation from the postulated equipartition increases the energy required to account for the observed luminosities. Some authors believe that the real demands on the energy source may be still higher because of the probable presence of high energy protons. The ratio Ep/Ee is determined by the way in which particles gain and lose energy, and it is impossible to estimate it a priori. Observationally one has two conflicting lines of evidence: (a) in galactic cosmic rays one measures (Ep/Ee) ≃ 102; (b) in the Crab Nebula one infers (Ep/Ee) ≲ 1 (otherwise the dynamical pressure of the proton gas would cause a nebular expansion much faster than observed).

Sign in / Sign up

Export Citation Format

Share Document