Use this URL to cite or link to this record in EThOS: https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.760478
Title: What can we learn from pulsar timing arrays (or not) : constraining astrophysical parametric models with gravitational waves
Author: Chen, Siyuan
ISNI:       0000 0004 7432 4681
Awarding Body: University of Birmingham
Current Institution: University of Birmingham
Date of Award: 2018
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Abstract:
Super massive black holes have been found in the centre of massive galaxies, which have also been observed to merge. Consequently, the central black holes should also form a binary and merge when their host galaxies collide. The galaxy merger rate can be calculated from astrophysical observables, such as the galaxy stellar mass function, pair fraction and merger time scale. Using galaxy - black hole relations it can be converted into a super massive black hole binary (SMBHB) merger rate, i.e. the population of SMBHBs in the Universe. Additionally, properties of individual SMBHBs, like their eccentricities and the densities of their stellar environment, also have an impact on the emission of gravitational waves (GWs). All the GWs emitted by the population of SMBHBs form a gravitational wave background (GWB), which is one of the prime targets for PTAs. Although, PTAs have not been able to detect such a background yet, stringent upper limits on the GWB have been produced. This thesis aims to investigate what we can learn from these upper limits as well as what could be learned from a detection.
Supervisor: Not available Sponsor: Institute of Physics ; Royal Astronomical Society ; University of Birmingham
Qualification Name: Thesis (Ph.D.) Qualification Level: Doctoral
EThOS ID: uk.bl.ethos.760478  DOI: Not available
Keywords: QB Astronomy ; QC Physics
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