Two Additions to the New Class of Low Accretion-Rate Magnetic Binaries

TL;DR

This paper reports the discovery of two new low accretion-rate magnetic white dwarf binaries, expanding the known class and providing insights into their accretion mechanisms and evolutionary status.

Contribution

It introduces two new low accretion-rate magnetic white dwarf binaries with detailed measurements, expanding the class and suggesting wind accretion as the dominant process.

Findings

Measured magnetic fields of 42 MG and 57 MG.

Accretion rates of 0.6-5x10^{-13} Msun/yr.

Most systems are likely pre-Polars with wind accretion.

Abstract

Two new magnetic white dwarf accretion binaries with extremely low mass-transfer rates have been discovered in the course of the Sloan Digital Sky Survey. Measured magnetic fields are 42 MG and 57 MG, and one system orbits with a period of just 82 min. The new systems therefore significantly expand the range in properties exhibited by the small class. The measured accretion rates are very low, 0.6-5x10^{-13} Msun/yr, and multiple visits spanning more than a year confirm that this is not a short-lived characteristic. It is becoming increasingly clear that the low-mdot magnetic white dwarf binaries accrete by nearly complete magnetic capture of the stellar wind from the secondary star rather than by Roche lobe overflow. The accretion rates therefore provide some of the first realistic estimates of the total wind loss rates from M dwarfs. Although one or more of the eight systems known to date may be interrupted or possibly even extinct Polars, several lines of evidence suggest that most are pre-Polars whose evolution has not yet brought the secondaries into contact with their Roche surfaces. Considering the difficulties of identifying binaries over a wide range in field strength and accretion rate, it is quite possible that the space density of wind-accreting magnetic binaries exceeds that of the classical X-ray emitting, Roche-lobe overflow Polars.