Fundamental Properties of Novae in M31

Abstract The peak luminosities and rates of decline for a large sample of novae recently published by Clark et al. have been analyzed using the Yaron et al. nova models to estimate fundamental properties of the M31 nova population. The apparent white dwarf (WD) mass distribution is approximately Gaussian with a mean 〈 M WD 〉 = 1.16 ± 0.14 M ⊙ . When corrected for recurrence time bias, the mean drops to 〈 M WD 〉 = 1.07 M ⊙ . The average WD mass of the M31 nova sample is found to be remarkably similar to that found by Shara et al. in their study of 82 Galactic novae but ∼0.15 M ⊙ more massive than the mean recently determined by Schaefer in his comprehensive study of more than 300 systems. As expected, the average WD mass for the recurrent novae included in the M31 sample, 〈 M WD 〉 = 1.33 ± 0.08 M ⊙ , is significantly higher than that for novae generally. Other parameters of interest, such as the accretion rate, velocity of the ejecta, and predicted recurrence time, are characterized by skewed distributions with large spreads about means of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">〈</mml:mo> <mml:mi>log</mml:mi> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mi mathvariant="normal">yr</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">)</mml:mo> <mml:mo stretchy="false">〉</mml:mo> <mml:mo>≃</mml:mo> <mml:mo>−</mml:mo> <mml:mn>9.27</mml:mn> </mml:math> , <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">〈</mml:mo> <mml:msub> <mml:mrow> <mml:mi>V</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">max</mml:mi> </mml:mrow> </mml:msub> <mml:mo stretchy="false">〉</mml:mo> <mml:mo>≃</mml:mo> <mml:mn>1690</mml:mn> </mml:math> km s −1 , and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">〈</mml:mo> <mml:mi>log</mml:mi> <mml:msub> <mml:mrow> <mml:mi>P</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">rec</mml:mi> </mml:mrow> </mml:msub> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi mathvariant="normal">yr</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mo stretchy="false">〉</mml:mo> <mml:mo>≃</mml:mo> <mml:mn>4.39</mml:mn> </mml:math> , respectively. The role of hibernation in affecting the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> </mml:math> and P rec distributions is briefly discussed. Finally, the nova properties were studied as a function of apparent position (isophotal radius) in M31, with the preponderance of evidence failing to establish any clear dependence on stellar population.