EDP Sciences
Free access
Volume 426, Number 1, October IV 2004
Page(s) L1 - L3
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200400071

A&A 426, L1-L3 (2004)
DOI: 10.1051/0004-6361:200400071


On the unpulsed radio emission from J0737-3039

R. Turolla1 and A. Treves2

1  Dipartimento di Fisica, Università di Padova, via Marzolo 8, 35131 Padova, Italy
    e-mail: turolla@pd.infn.it
2  Dipartimento di Fisica e Matematica, Università dell'Insubria, via Valleggio 11, 22100 Como, Italy

(Received 15 June 2004 / Accepted 6 September 2004 )

The double pulsar system J0737-3039 appears associated with a continuous radio emission, nearly three times stronger than that of the two pulsars together. If such an emission comes from a transparent cloud its spatial extent ( $\ga$ $10^{13}~{\rm
cm}$ ) should be substantially larger than the orbital separation. Assuming homogeneity and equipartition, the cloud magnetic field is ~ $0.03~{\rm G}$ and the electron characteristic energy ~ $60~{\rm MeV}$. This is consistent with supposing that relativistic electrons produced in the shock formed by the interaction of the more luminous pulsar wind with the magnetosphere of the companion flow away filling a larger volume. Alternatively, the unpulsed emission may directly come from the bow shock if some kind of coherent mechanism is at work. Possible observational signatures that can discriminate between the two pictures are shortly discussed.

Key words: pulsars: individual: PSR J0737-3039A/B -- radiation mechanisms: non-thermal -- stars: neutron

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© ESO 2004