Max-Planck-Institut für Radioastronomie Towards Improving and Understanding the Timing of PSR J0737–3039B Aristeidis Noutsos MPIfR Collaborators: G. Desvignes, M. Kramer, N. Wex, P . C. C. Freire, I. H. Stairs, M. A. McLaughlin, R. N. Manchester, A. Possenti, M. Burgay, A. G. Lyne, R. P . Breton, and B. B. P . Perera XIV Bonn NS workshop, MPIfR, Bonn 17.02.2020
The Double Pulsar The only system we know to date, where L we observe pulsed emission from both NSs S B S A P b ≈ 2.4 h P B = 2.77 s P A = 22.7 ms Kramer & Stairs (2008) ascending node Magnetosheath Pulsar A brightness Pulsar B Wind from A pulsar wind magnetosheath IP Magnetosphere of B To Earth B BP2 to Earth A L WP i B g h t c y l i n d e r BP1 • Pulsar A distorts Pulsar B’s magnetosphere with its relativistic particle wind • Pulsar A is sill visible and a very stable timer • Pulsar B: precessed out of view in 2008 e.g. Breton et al. (2008)
<latexit sha1_base64="dF7BIKPHhm5linG9IOI2OHoTqI8=">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</latexit> <latexit sha1_base64="dF7BIKPHhm5linG9IOI2OHoTqI8=">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</latexit> <latexit sha1_base64="dF7BIKPHhm5linG9IOI2OHoTqI8=">AChHicfVHLSgMxFM2M7/qutRFsCgutEzUqhvFx8alglXB1J0xpMJkOSUcswW/RL3DjR5gZB9FWvBA4nHvOeTcMBbc2CB48/yR0bHxicmpyvTM7Nx8dWHx2qhEU9akSih9GxLDBI9Y03Ir2G2sGZGhYDfh41nev3li2nAVXdl+zFqS9CLe5ZRYR7Wry/3KdYSqtBk7QKdZOuHqL6LGsHONsSxhE9yAtBDPEmLGawDNVLKuyWyTKIcWVI5LQaA9C2B9v4RaFdrpU0AhwEqQ2UdGuvuOolkaWCGHOHgti2UqItp4JlFZwYFhP6SHrszsGISGZaZFXBtc04Fdpd2LCzYnxspkcb0ZegmJbEPZrCXk3/2nonpu8UBe9s9aKU8ihPLIvrl3k0EtArmF4Edrhm1ou8AoZq7D0D6QDSh1t0tTwYN5jAMrfrKijy93a8WmZ0SRYBqtgAyCwD47BObgATUDBh7foLXsr/ri/6e/4ja9R3yt3lsCv8o8+Afv+vN4=</latexit> <latexit sha1_base64="dF7BIKPHhm5linG9IOI2OHoTqI8=">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</latexit> Timing … and across each bright phase Strong profile evolution across the orbit … MJD 53400–53500 MJD 53400–53500 10 10 BP1 9 9 BP1 8 8 Flux density (mJy) 7 Flux density (mJy) 7 6 6 5 5 4 4 BP2 3 3 2 2 IP WP 1 1 0 0 –0.25 –0.2 –0.15 –0.1 –0.05 0 0.05 0.1 0.15 0.2 0.25 –0.05 0 0.05 0.1 0.15 0.2 0.25 0.3 0.35 Pulse phase Pulse phase This results in poor timing precision , due to systematics Pulsar A is a great timer in comparison =3 x obs = 1 . 415032 ± 0 . 000001 lt-s bright phases (BPs) A x obs = 1 . 5161 ± 0 . 0016 lt-s weak phase (WP) B (Kramer et al. 2006)
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For a wide range of gravity theories, we can express the PK parameters as a function of the Keplerian parameters and m A and m B : Kramer et al. (in preparation) GR p PK = f i ( p K ; m A , m B ) i A common intersection of all f i at the binary’s masses implies that the theory is correct . R = x int = m B is: A x int m A B • theory independent • poorly constrained due to Pulsar B timing * * the precision of the rest of the PK parameters improves with more Pulsar A data Improving Pulsar B timing will improve the precision of GR tests with this system
Pulsar B Data Our data: • Observations with the GBT at 820 MHz and with Parkes at 685 MHz and 1.4 GHz . • Data span ≈ 4 years (2004 – 2008) • After data selection and RFI excision: 4,115 profiles (flux-calibrated) • To map the precessional evolution, we binned the data into 15 100-day intervals ~15 ′ 2.5h Short-term quasi-linear drifts across each of the BPs harmonic drift as a function of orbital phase ~4yr long-term modulation of the harmonic drift’s amplitude no data
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