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| pulsar B1937+21 | |
|---|---|
| Name | B1937+21 |
| Type | Pulsar |
| Epoch | J2000 |
| Ra | 19h 39m 38.561s |
| Dec | +21° 34′ 59.14″ |
| Period | 1.5578 ms |
| Distance | ~3.6 kpc |
| Constellation | Vulpecula |
pulsar B1937+21 is a millisecond pulsar located in the constellation Vulpecula, notable for being the first discovered sub-2-ms radio pulsar and among the fastest-spinning neutron stars known. Its discovery transformed studies of radio astronomy, neutron stars, and pulsar timing and tied into broader programs at institutions such as Arecibo Observatory, Green Bank Observatory, and Jodrell Bank Observatory. The object has been central to work on General relativity, Binary pulsar dynamics, and precision timekeeping initiatives connected to projects like the International Pulsar Timing Array and the European Pulsar Timing Array.
B1937+21 was identified in a survey using the Arecibo Observatory receiver systems during an era of rapid development in Radio telescope technology and signal processing led by teams from Cornell University, National Radio Astronomy Observatory, and collaborators at Stanford University. The initial detection was contemporaneous with studies at Jodrell Bank Observatory and followed methods pioneered in programs at Cambridge Observatory and by researchers associated with Princeton University and University of California, Berkeley. Early identification involved distinguishing its ultra-short period from terrestrial interference and required expertise similar to that applied in surveys at Mount Pleasant Observatory and Molonglo Observatory Synthesis Telescope.
The pulsar rotates with a period near 1.5578 milliseconds, making it comparable to other rapid rotators discovered subsequently at Parkes Observatory and in searches using Effelsberg Radio Telescope. Precision timing campaigns have tied its rotational stability to efforts by teams at MIT, Caltech, and NASA laboratories, linking measurements to standards maintained by institutions like National Institute of Standards and Technology. Long-term timing reveals tiny spin-down rates that informed models at Max Planck Institute for Radio Astronomy and constrained torque processes studied at University of Manchester and Harvard-Smithsonian Center for Astrophysics.
The pulse profile shows extremely narrow components and giant-pulse phenomena investigated alongside studies of Crab Pulsar emission, work led by groups at Columbia University and Rutgers University. Spectral observations spanning facilities including Very Large Array, Westerbork Synthesis Radio Telescope, and Sardinia Radio Telescope linked its radio spectrum and polarization characteristics to theoretical frameworks developed at Princeton Plasma Physics Laboratory and the Max Planck Society. High-time-resolution data collected by teams at University of California, Santa Cruz and Northwestern University revealed microstructure and subpulse modulation analogous to features studied in pulsars at University of Toronto and McGill University.
Although many millisecond pulsars reside in binaries discovered in surveys by European Southern Observatory and National Astronomical Observatory of Japan, this object is effectively isolated, prompting comparisons with isolated millisecond pulsars found in globular clusters studied at Space Telescope Science Institute and European Space Agency programs. Its local interstellar environment has been probed using dispersion and scattering analyses conducted by researchers affiliated with Columbia University, University of Wisconsin–Madison, and University of British Columbia, linking propagation effects to electron density models developed at Harvard University and Ohio State University.
Interpretations of its emission invoke magnetospheric models advanced at University of Oxford, Dublin Institute for Advanced Studies, and University of Tokyo, and draw on plasma physics concepts explored at Lawrence Livermore National Laboratory and Princeton University. Studies comparing polar-cap, outer-gap, and slot-gap scenarios involved collaborations with theorists at Stanford University, Massachusetts Institute of Technology, and University of Chicago, and benefited from particle-in-cell simulations produced by groups at Los Alamos National Laboratory and Argonne National Laboratory.
Observations have exploited backend instruments and receivers developed by teams at Arecibo Observatory, Green Bank Observatory, Parkes Observatory, and Jodrell Bank Observatory, with digital signal processing advances contributed by engineers at National Radio Astronomy Observatory, CSIRO, and MIT Haystack Observatory. International monitoring included campaigns supported by European Southern Observatory, National Astronomical Observatory of Japan, and National Science Foundation grants, while multiwavelength follow-up involved satellites such as Chandra X-ray Observatory, Fermi Gamma-ray Space Telescope, and XMM-Newton used by scientists at NASA Goddard Space Flight Center and European Space Agency centers.
The pulsar's extreme rotation period provided stringent constraints used in tests of General relativity and in searches for low-frequency Gravitational wave backgrounds conducted by the International Pulsar Timing Array, North American Nanohertz Observatory for Gravitational Waves, and the European Pulsar Timing Array. Its timing precision informed work on neutron-star equation of state by researchers at Institute for Advanced Study, Los Alamos National Laboratory, and Kavli Institute for Theoretical Physics, and contributed to developments in precision timekeeping that intersect with standards from National Institute of Standards and Technology and techniques employed at Jet Propulsion Laboratory.
Category:Pulsars