Richard Van Evera Lovelace

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Richard Van Evera Lovelace is an American astrophysicist and plasma physicist. Lovelace is the best known for discovery of period of \href{}pulsar in \href{}{Crab Nebula} (\href{}{Crab pulsar}), which helped to prove that pulsars are rotating \href{}
{neutron stars}, for developing a magnetic model of \href{}{jets from galaxies}, and for developing a model of 
\href{,the%20rotation%20of%20the%20planet.}{Rossby waves} in \href{}{accretion disks}. He organized the \href{}{US-Russia collaboration in Plasma Astrophysics}, which obtained many pioneering results in modeling of plasma accretion and outflows from magnetized rotating stars.

Richard Lovelace ([[]]) is astrophysicist at the Cornell University [1].

Pulsars and Neutron stars

1969, Lovelace and his coauthors suggest interpretation of the already discovered pulsar (Crab nebula pulsar NP 0532) as rotating neutorn stars, that emit narrow beam of radiowaves.[2] Soon after his suggestion, such an interpretation had been confirmed [3]


  1. Richard VE Lovelace Professor, Departments of Astronomy and Applied and Engineering Physics, Cornell University. (2020)
  2. Crab nebula pulsar NP 0532 J.M.Comella, H.D.Craft, R.V.E.Lovelace, J.M.Sutton, G.Leonard Tyler Nature Volume 221 Issue 5179 Pages 453-454 Publication date 1969/2/1 BECAUSE of the conjecture that pulsars are neutron stars, which are possibly produced in supernova events, the possible association of pulsars with supernova remnants is of great interest. Staelin and Reifenstein recently reported1 the discovery of two pulsed radio sources near the Crab nebula, which is the remnant of the supernova observed by the Chinese in AD 1054. Pulses from both sources were described as very sporadic, and no periodic phenomena were evident.
  3. Private communication. 2020. A neutron star is the collapsed core of a massive supergiant star, which had a total mass of between 10 and 25 solar masses, possibly more if the star was especially metal-rich.[1] Neutron stars are the smallest and densest stellar objects, excluding black holes and hypothetical white holes, quark stars, and strange stars.[2] Neutron stars have a radius on the order of 10 kilometres (6.2 mi) and a mass of about 1.4 solar masses.[3] They result from the supernova explosion of a massive star, combined with gravitational collapse, that compresses the core past white dwarf star density to that of atomic nuclei. A pulsar (from pulse and -ar as in quasar)[1] is a highly magnetized rotating compact star (usually neutron stars but also white dwarfs) that emits beams of electromagnetic radiation out of its magnetic poles.[2] This radiation can be observed only when a beam of emission is pointing toward Earth (much like the way a lighthouse can be seen only when the light is pointed in the direction of an observer), and is responsible for the pulsed appearance of emission. Neutron stars are very dense, and have short, regular rotational periods. This produces a very precise interval between pulses that ranges from milliseconds to seconds for an individual pulsar. Pulsars are one of the candidates for the source of ultra-high-energy cosmic rays (see also centrifugal mechanism of acceleration). // The periods of pulsars make them very useful tools for astronomers. Observations of a pulsar in a binary neutron star system were used to indirectly confirm the existence of gravitational radiation. The first extrasolar planets were discovered around a pulsar, PSR B1257+12. In 1983, certain types of pulsars were detected that at that time exceeded atomic clocks in their accuracy in keeping time.[3]


Cornell Univercity, Ion ring, Neutron star, Pulsar, Richard Lovelace, Scholar