Baylin , C.D. 1987, PhD Thesis Eggleton , P.. & Kiseleva , L., 1995, ApJ 455,640

1. Formation of the Triple Millisecond Pulsar with two white dwarf companions PSR J0337+1715 ApJ.Letters 781, L13,2014 Contacts: tauris@astro.uni-bonn.de E.P.J.vandenheuvel@uva.nl Thomas Tauris ¹ andEd P.J. van den Heuvel² 1. UniversitatBonn, Argelander Institute for Astronomy (DE), and Max Planck Institute for Radio Astronomy, Bonn (DE); 2. Anton Pannekoek Institute, University of Amsterdam (the Netherlands) 4 The masses of the twowhitedwarfsvery well fit the theoretical White DwarfMass-Orbital period relationfor Helium WDsleftbehindfromevolved Roche-lobefilling donor stars in Low-Mass X-rayBinaries . This means that the system went throughtwo Low-Mass X-rayBinaryphases. Measurement of the system velocitywill, accordingtoourcalculations, allowto put constraints on the kick velocitywimpartedto the neutron star duringitsbirth in the supernova explosion, as follows: The second figurefigure in the right-hand column togetherwith the abovetable shows: Baylin, C.D. 1987, PhD Thesis Eggleton, P.. & Kiseleva, L., 1995, ApJ 455,640 Harrington, R.S. 1972, Celestial Mechanics, 6, 322. Mardling, R.A. & Aarseth, S.J. 2001,MNRAS 321,308. Tauris,T. & Savonije, G.J. 1999, A&A 350,928. References