- #1
Saul
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It is interesting to compare pulsars to quasars. If one assumes the massive compact object at the center of a quasar is a physical object that has properties, is it similar to what creates the pulsar and magstar observations? What are the pulsar and magstar observations? What are the quasar observations? There do appear to be similarities.
The pulsar observations, the quasar observations, and magstar observations are different from what one might assume based on the cartoon pictures in textbooks. The explanation of these differences is included in recently published papers.
This paper was included as recommended reading at a presentation made at a pulsar conference for specialists in that field.
F. C. Michel alleges that due to more sophisticated Earth and space based telescopes there is now sufficient observational evidence to make progress in pulsar theory. Michel alleges in this paper that one obstacle to advancement in pulsar astrophysics is that specific theoretical models when they are included in textbooks and taught fix the thinking concerning this subject. Michel alleges that observational evidence and holistic critical fundamental physical analysis of the textbook models in question shows that they are fundamentally incorrect.
Michel's point is there was no rational reason to present the pulsar textbook model as the correct model. The class of pulsar model that he alleges may lead to a solution was postulated in the 1960s.
http://arxiv.org/PS_cache/astro-ph/pdf/0308/0308347v1.pdf
The pulsar observations, the quasar observations, and magstar observations are different from what one might assume based on the cartoon pictures in textbooks. The explanation of these differences is included in recently published papers.
This paper was included as recommended reading at a presentation made at a pulsar conference for specialists in that field.
F. C. Michel alleges that due to more sophisticated Earth and space based telescopes there is now sufficient observational evidence to make progress in pulsar theory. Michel alleges in this paper that one obstacle to advancement in pulsar astrophysics is that specific theoretical models when they are included in textbooks and taught fix the thinking concerning this subject. Michel alleges that observational evidence and holistic critical fundamental physical analysis of the textbook models in question shows that they are fundamentally incorrect.
Michel's point is there was no rational reason to present the pulsar textbook model as the correct model. The class of pulsar model that he alleges may lead to a solution was postulated in the 1960s.
http://arxiv.org/PS_cache/astro-ph/pdf/0308/0308347v1.pdf
The State of Pulsar Theory
However, recent theoretical work is converging on a picture that closely resembles the latest HST and CHANDRA images, providing hope for the future. No less than 3 groups have recently confirmed the early Krause-Polstorff-Michel simulations showing that the fundamental plasma distribution around a rotating neutron star consists of two polar domes and an equatorial torus of trapped nonneutral plasma of opposite sign charges. Unless a lot of new physics can be added, this distribution renders the Goldreich-Julian model irrelevant (i.e., along with most of the theoretical publications over the last 33 years).
So 35 years have passed. Will the way pulsars work yield to theory alone? Will it yield to observation alone? The numbers are not on anyone’s side. I will try to suggest why theory hasn’t done it yet. One reason was the chaotic approach to the problem, everyone running in different directions. The other is, paradoxically, how a strong line of conventional wisdom keeps people from looking in different directions, which we will next examine.
Pair production
The possible role of pair production has been an interesting one, and we find it very attractive (Michel 1991b) because it could explain how charged bunches would form naturally and thereby account for the coherency of pulsar radiation. One role of pair production might be to provide ionization outside of the neutron star and thereby help “fill” the magnetosphere as imagined in the GJ model (although these authors were clear in their assumption that the magnetospheric particles all came from the surface). Although something like this should be possible (owing to the huge E* B ≠ 0 regions between the domes and the tori) STM (2001) show that the consequent filling of the domes and tori reduce this source and would turn it off. Moreover, for typical pulsars where the magnetic field at the famous light cylinder would be only of the order of a few gauss, pair production would have no chance of operating. Pair production was suggested in the first place only because the pulsar magnetic fields were so large at the surface.
Nonneutral Plasmas
Most astrophysicists or physicists are not taught nonneutral plasmas. There are relatively few sources Davidson (1990), Michel and Li (1999), Michel (1982, 1991a). Yet nonneutral plasmas are the natural plasmas to be found around strongly electrified objects like rotating neutron stars, simply because the huge electric fields tend to stratify the plasma (as in producing domes and tori) and selectively pull out plasma (from conducting surfaces) of only one sign. The fact that the plasma surrounding a rotating magnetized neutron star should be arranged in the form of domes and tori should be understood as a fundamental one which would have to be explicitly modified if one were to find a structurally different configurations (such as accelerating gaps over the polar caps) instead of simply being ignored because it doesn’t fit preconception.
Danger when theorists start looking at the same page
Theorists seem uninterested in why 35 years have passed with so little success. Not even interested enough when it can be shown that the favorite model is a cartoon model not based on real physics. The possible bad news here is that a number of other people have now become interested in how nonneutral plasmas impact our understanding of pulsars. Then everyone might have to learn this stuff!