Σύγκριση μεθόδων

	Συστοιχία Χρονισμού Πάλσαρ	Κινηματική Απόσταση
Πεδίο	Αστρονομία	Αστρονομία
Οικογένεια	Process / pipeline	Process / pipeline
Έτος προέλευσης	1979	1957
Δημιουργός	Stephen Detweiler	Bert Westerhout
Τύπος	Observational timing method	Kinematic measurement method
Θεμελιώδης πηγή	Sazhin, M. V. (1978). Opportunities for detecting ultralong gravitational waves. Soviet Astronomy, 22, 36-38.	Reid, M. J., et al. (2014). Trigonometric parallaxes of high mass star forming regions: the structure and kinematics of the Milky Way. Astrophysical Journal, 783(2), 130.
Εναλλακτικές ονομασίες	PTA, Millisecond Pulsar Timing, Pulsar Timing Residuals	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax
Συναφείς	3	3
Σύνοψη	A pulsar timing array uses multiple millisecond pulsars as a distributed network of gravitational wave detectors across the galaxy. Proposed theoretically by Stephen Detweiler in 1979, this method exploits the extraordinary timing precision of pulsars to detect the subtle spacetime distortions caused by gravitational waves. In 2023, the first evidence for a stochastic background of gravitational waves was announced using pulsar timing arrays.	Kinematic distance is a method for estimating distances to objects in the Milky Way using their observed radial velocities and the known rotation curve of the Galaxy. Developed in the 1950s by Bert Westerhout and others, this technique enables distance determination to distant molecular clouds and masers without trigonometric parallax or individual object luminosities.