Author ORCID Identifier

Phukon, khun Sang AAY-4869-2021 Favata, Marc AAA-6755-2022 Samajdar, Anuradha AAA-3165-2022 Nelemans, Gijs D-3177-2012 Mapelli, Michela ABA-4708-2020 Bertolini, Alessandro ABG-4851-2021 SHCHEBLANOV, Nikita D-3713-2011 Marquina, Antonio F-8755-2012 Arun, K G CARAPELLA, Giovanni Chiadini, Francesco E-1812-2015 Coward, David Jones, Aaron Ejlli, Aldo Jaranowski, Piotr Helmling-Cornell, Adrian Ho, Wynn Pan, Kuo-Chuan Bassiri, Riccardo Mow-Lowry, Conor F-8843-2015 Karki, Sudarshan Sun, Ling Hill, Paul Naticchioni, Luca AAB-7775-2019 Gergely, Laszlo Arpad X-7693-2018 Cieslar, Marek Edelman, Bruce Sintes, Alicia M Stuver, Amber L-9985-2018 Kovalam, Manoj Blair, Carl Nakano, Hiroyuki Anderson, Warren Bejger, Michal Mondin, Marina Zeidler, Simon Strang, Lucy Park, June Gyu Pitkin, Matthew I-3802-2013 Kakizaki, Mitsuru Charlton, Philip Parisi, Alessandro MARTINEZ, MARIO I-3549-2015 Buscicchio, Riccardo Itoh, Yousuke Ciecielag, Pawel Sanchis-Gual, Nicolas , Tejinder Kaur Sorrentino, Nunziato Espinoza, Cristobal U-4428-2017 Kuroyanagi, Sachiko B-3843-2017 Kumar, Prayush Thrane, Eric Poggiani, Rosa Kong, Albert Singh, Neha Rozza, Davide Nishizawa, Atsushi Garufi, Fabio K-3263-2015 Hollows, Ian Hannuksela, Otto Akseli Leonardi, Matteo G-9694-2015 Shao, Lijing Costa, Cesar G-7588-2012 Plastino, Wolfango Zhao, Yuhang

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We present a search for continuous gravitational-wave emission due to r-modes in the pulsar PSR J0537-6910 using data from the LIGO-Virgo Collaboration observing run O3. PSR J0537-6910 is a young energetic X-ray pulsar and is the most frequent glitcher known. The inter-glitch braking index of the pulsar suggests that gravitational-wave emission due to r-mode oscillations may play an important role in the spin evolution of this pulsar. Theoretical models confirm this possibility and predict emission at a level that can be probed by ground-based detectors. In order to explore this scenario, we search for r-mode emission in the epochs between glitches by using a contemporaneous timing ephemeris obtained from NICER data. We do not detect any signals in the theoretically expected band of 86-97 Hz, and report upper limits on the amplitude of the gravitational waves. Our results improve on previous amplitude upper limits from r-modes in J0537-6910 by a factor of up to 3 and place stringent constraints on theoretical models for r-mode-driven spin-down in PSR J0537-6910, especially for higher frequencies at which our results reach below the spin-down limit defined by energy conservation.

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Other LSU authors:

C. Austin; H. W. Cain, III; L. Cohen; T. R. Corbitt; T. J. Cullen; J. Glanzer; G. Gonzalez; A. R. Guimaraes; T. Hardwick; M. L Lollie; S. Soni; A. L. Urban

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