Jove
Visualize
Contact Us

Related Experiment Videos

Gravitational-wave stochastic background from cosmic strings.

Xavier Siemens1, Vuk Mandic, Jolien Creighton

  • 1Center for Gravitation and Cosmology, Department of Physics, University of Wisconsin-Milwaukee, P.O. Box 413, Milwaukee, Wisconsin 53201, USA.

Physical Review Letters
|May 16, 2007
PubMed
Summary

Cosmic string gravitational waves are detectable by current detectors like LIGO, complementing other cosmic observations. Future detectors will probe more cosmic string model parameters.

Related Concept Videos

You might also read

Related Articles

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

Sort by
Same author

Two-Step Procedure to Detect Cosmological Gravitational Wave Backgrounds with Next-Generation Terrestrial Gravitational-Wave Detectors.

Physical review letters·2025
Same author

Criteria for identifying and evaluating locations that could potentially host the Cosmic Explorer observatories.

The Review of scientific instruments·2025
Same author

Low-latency gravitational wave alert products and their performance at the time of the fourth LIGO-Virgo-KAGRA observing run.

Proceedings of the National Academy of Sciences of the United States of America·2024
Same author

Detection of early-universe gravitational-wave signatures and fundamental physics.

General relativity and gravitation·2022
Same author

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

Physical review letters·2022
Same author

Site-selection criteria for the Einstein Telescope.

The Review of scientific instruments·2020
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

Area of Science:

  • Cosmology and astrophysics
  • Gravitational wave astronomy

Background:

  • Cosmic strings are hypothetical topological defects formed during phase transitions in the early universe.
  • These strings can generate a stochastic background of gravitational waves.
  • Understanding this background provides insights into fundamental physics and early universe cosmology.

Purpose of the Study:

  • To investigate the stochastic gravitational wave background from cosmic strings.
  • To assess the detectability of this background by current and future gravitational wave observatories.
  • To compare the sensitivity of gravitational wave detectors with existing cosmological constraints (Big Bang Nucleosynthesis, Cosmic Microwave Background, pulsar timing).

Main Methods:

  • Theoretical modeling of gravitational wave emission from cosmic string networks.

Related Experiment Videos

  • Analysis of sensitivity curves for current (LIGO) and planned (Advanced LIGO, LISA) gravitational wave detectors.
  • Comparison with established astrophysical and cosmological constraints.

    • Main Results:

    • Current Laser Interferometer Gravitational Wave Observatory (LIGO) data are sensitive to cosmic string parameter space not covered by pulsar timing, Big Bang Nucleosynthesis (BBN), and Cosmic Microwave Background (CMB) constraints.
    • Gravitational wave detectors offer complementary sensitivity to cosmic string models.
    • Future detectors like Advanced LIGO and Laser Interferometer Space Antenna (LISA) will significantly expand the explored parameter space.

    Conclusions:

    • Gravitational wave astronomy provides a unique window into cosmic string physics.
    • Interferometric detectors are crucial for probing specific regions of cosmic string parameter space.
    • Continued advancements in gravitational wave detection will enhance our understanding of early universe phenomena.