Jove
Visualize
Contact Us
JoVE
x logofacebook logolinkedin logoyoutube logo
ABOUT JoVE
OverviewLeadershipBlogJoVE Help Center
AUTHORS
Publishing ProcessEditorial BoardScope & PoliciesPeer ReviewFAQSubmit
LIBRARIANS
TestimonialsSubscriptionsAccessResourcesLibrary Advisory BoardFAQ
RESEARCH
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchive
EDUCATION
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualFaculty Resource CenterFaculty Site
Terms & Conditions of Use
Privacy Policy
Policies

Related Concept Videos

NMR Spectrometers: Radiofrequency Pulses and Pulse Sequences01:17

NMR Spectrometers: Radiofrequency Pulses and Pulse Sequences

1.9K
A pulse is a short burst of radio waves distributed over a range of frequencies that simultaneously excites all the nuclei in the sample. Upon passing a radio frequency pulse along the x-axis, the nuclei absorb energy corresponding to their Larmor frequencies and achieve resonance. This shifts the net magnetization vector from the z-axis toward the transverse plane. This angle of rotation of the magnetization vector, or the flip angle, is proportional to the duration and intensity of the pulse.
1.9K
Atomic Nuclei: Larmor Precession Frequency01:11

Atomic Nuclei: Larmor Precession Frequency

3.3K
The earth's gravitational field produces a 'twisting force' perpendicular to the angular momentum of a spinning mass (such as a spinning top) that causes the mass to 'wobble' around the gravitational field axis in a phenomenon called precession. Similarly, the magnetic moment (μ) of a spinning nucleus precesses due to an external magnetic field directed along the z-axis. The precession of the magnetic moment vector about the magnetic field is called Larmor precession,...
3.3K
Detection of Black Holes01:10

Detection of Black Holes

2.6K
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
2.6K
¹H NMR Signal Multiplicity: Splitting Patterns01:13

¹H NMR Signal Multiplicity: Splitting Patterns

7.5K
When protons A and X are coupled, their nuclear spin energy levels are slightly modified. This is because the energy required to excite proton A to a spin state parallel to proton X is slightly different from the energy required for it to become anti-parallel to spin X. Consequently, there are two possible excitation frequencies for A (A1 and A2), depending on the spin state of X, and vice versa. The mutual nature of coupling implies that the difference between frequencies A1 and A2, indicated...
7.5K
Atomic Nuclei: Nuclear Spin State Population Distribution01:14

Atomic Nuclei: Nuclear Spin State Population Distribution

2.5K
Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
2.5K
Atomic Nuclei: Nuclear Relaxation Processes01:23

Atomic Nuclei: Nuclear Relaxation Processes

1.3K
In the absence of an external magnetic field, nuclear spin states are degenerate and randomly oriented. When a magnetic field is applied, the spins begin to precess and orient themselves along (lower energy) or against (higher energy) the direction of the field. At equilibrium, a slight excess population of spins exists in the lower energy state. Because the direction of the magnetic field is fixed as the z-axis,  the precessing magnetic moments are randomly oriented around the z-axis.
1.3K

You might also read

Related Articles

Articles linked to this work by shared authors, journal, and citation graph.

Sort by
Same author

Searching for Gravitational Waves from Cosmological Phase Transitions with the NANOGrav 12.5-Year Dataset.

Physical review letters·2022
Same author

Universality of free fall from the orbital motion of a pulsar in a stellar triple system.

Nature·2018
Same author

Binary and Millisecond Pulsars at the New Millennium.

Living reviews in relativity·2017
Same author

Binary and Millisecond Pulsars.

Living reviews in relativity·2017
Same author

A radio pulsar/x-ray binary link.

Science (New York, N.Y.)·2009
Same author

An eccentric binary millisecond pulsar in the galactic plane.

Science (New York, N.Y.)·2008
Same journal

Primordial black holes and their gravitational-wave signatures.

Living reviews in relativity·2025
Same journal

Solvable models of quantum black holes: a review on Jackiw-Teitelboim gravity.

Living reviews in relativity·2023
Same journal

Electromagnetic counterparts to massive black-hole mergers.

Living reviews in relativity·2022
Same journal

Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA.

Living reviews in relativity·2020
Same journal

Kilonovae.

Living reviews in relativity·2019
Same journal

Erratum: Publisher Correction: Interferometer techniques for gravitational-wave detection.

Living reviews in relativity·2019
See all related articles

Related Experiment Video

Updated: Mar 7, 2026

Generation and Coherent Control of Pulsed Quantum Frequency Combs
06:42

Generation and Coherent Control of Pulsed Quantum Frequency Combs

Published on: June 8, 2018

9.8K

Binary and Millisecond Pulsars.

Duncan R Lorimer1

  • 1Department of Physics, West Virginia University, P.O. Box 6315, Morgantown, WV 26506 USA.

Living Reviews in Relativity
|February 10, 2017
PubMed
Summary
This summary is machine-generated.

Recent surveys have expanded the catalog of known radio pulsars to over 1800, including numerous binary and millisecond pulsars in our Galaxy and globular clusters. Key discoveries include relativistic binary systems and massive pulsars.

More Related Videos

Preparing an Isotopically Pure 229Th Ion Beam for Studies of 229mTh
10:42

Preparing an Isotopically Pure 229Th Ion Beam for Studies of 229mTh

Published on: May 3, 2019

7.4K
Automation of Mode Locking in a Nonlinear Polarization Rotation Fiber Laser through Output Polarization Measurements
14:18

Automation of Mode Locking in a Nonlinear Polarization Rotation Fiber Laser through Output Polarization Measurements

Published on: February 28, 2016

12.0K

Related Experiment Videos

Last Updated: Mar 7, 2026

Generation and Coherent Control of Pulsed Quantum Frequency Combs
06:42

Generation and Coherent Control of Pulsed Quantum Frequency Combs

Published on: June 8, 2018

9.8K
Preparing an Isotopically Pure 229Th Ion Beam for Studies of 229mTh
10:42

Preparing an Isotopically Pure 229Th Ion Beam for Studies of 229mTh

Published on: May 3, 2019

7.4K
Automation of Mode Locking in a Nonlinear Polarization Rotation Fiber Laser through Output Polarization Measurements
14:18

Automation of Mode Locking in a Nonlinear Polarization Rotation Fiber Laser through Output Polarization Measurements

Published on: February 28, 2016

12.0K

Area of Science:

  • Astronomy and Astrophysics
  • Radio Pulsar Research

Background:

  • The known pulsar population has significantly increased due to recent successful surveys.
  • Over 1800 pulsars are now cataloged, with a substantial number being binary and millisecond pulsars.

Purpose of the Study:

  • To review the key properties, demographics, and applications of binary and millisecond radio pulsars.
  • To highlight recent advancements and discoveries in pulsar research.

Main Methods:

  • Review of observational data from recent pulsar surveys.
  • Analysis of pulsar properties, including mass, orbital parameters, and relativistic effects.

Main Results:

  • Catalog now includes 83 binary/millisecond pulsars in the Galactic disk and 140 in 26 globular clusters.
  • Discovery of the young relativistic binary PSR J1906+0746.
  • Identification of pulsars with masses exceeding 1.5 solar masses in globular clusters.
  • Precise measurement of relativistic spin precession in a double pulsar system.
  • Discovery of a Galactic millisecond pulsar in an eccentric orbit (e = 0.44) around an unevolved companion.

Conclusions:

  • Recent advancements have greatly enhanced our understanding of binary and millisecond pulsars.
  • Pulsar research, particularly in globular clusters, is experiencing a resurgence with significant discoveries.