A Triple Star Origin For T Pyx and Other Short-Period Recurrent Novae
C. Knigge, S. Toonen, T.C.N. Boekholt

TL;DR
This paper proposes that short-period recurrent novae like T Pyxidis originate from hierarchical triple star systems, where three-body dynamics induce eccentricity and mass transfer, explaining their unusual evolution.
Contribution
It introduces a novel triple star evolution scenario for short-period recurrent novae, supported by numerical simulations showing how triple dynamics trigger mass transfer.
Findings
Hierarchical triples can produce eccentric inner binaries leading to mass transfer.
Numerical models demonstrate triple evolution can produce observed short-period novae.
T Pyxidis likely evolved from a triple system, explaining its peculiar properties.
Abstract
Recurrent novae are star systems in which a massive white dwarf accretes material at such a high rate that it undergoes thermonuclear runaways every 1 - 100 years. They are the only class of novae in which the white dwarf can grow in mass, making some of these systems strong Type Ia supernova progenitor candidates. Almost all known recurrent novae are long-period (P_orb > 12 hrs) binary systems in which the requisite mass supply rate can be provided by an evolved (sub-)giant donor star. However, at least two recurrent novae are short-period (P_orb < 3 hrs) binaries in which mass transfer would normally be driven by gravitational radiation at rates 3-4 orders of magnitude smaller than required. Here, we show that the prototype of this class -- T Pyxidis -- has a distant proper motion companion and therefore likely evolved from a hierarchical triple star system. Triple evolution can…
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