Populations and properties of classical and recurrent novae in M31mjd/talks/COSPAR2018.pdf · 2019. 11. 8. · All quiescent novae with high M_ or giant donors can be recovered in

Populations and properties of classicaland recurrent novae in M 31

M. J. Darnley & M. Henze

Liverpool John Moores University & San Diego State University

July 19, 2018

Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 1 / 29

Outline

1 History — One Hundred Years of Survey-tude

2 Three hundred’s a crowd — Building Population Studies

3 Multi-Wavelength Views and Correlations

4 Interface with Theoretical Models

5 Recurrent Novae — The Fast and the Furious

6 M31N 2008-12a — Pushing the Boundaries

7 The Future of Extragalactic Nova Science


History — Hubble’s Survey of M 31


History — First observational trends & correlations

“Life-time vs luminosity” relation:

McLaughlin 1945, della Valle & Duerbeck 1993Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 6 / 29

Optical surveys — Two Populations?

Two taxonomic spectroscopic‘classes’: He/N vs Fe ii(+ hybrids & Ne)

Two distinct populations:bulge (‘old’) & disk (‘young’)1

Galactically: fast novae closerto the plane than slow novae2

– recently questioned3

M 31 bulge nova rate ∼ 5×larger than disk rate4

1Duerbeck 1990, 2della Valle 1992, 3Özdönmez+ 2018, 4Darnley+2006Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 7 / 29

Optical Surveys — Two Populations?

Age or metallicitydependence?

MW: ∼ 80% Fe ii1M 31: 82% Fe ii2

M 33: 25% Fe ii3

LMC: 50% Fe ii4

M 31 — based on 91 novae2:

No evidence for spectralclass dependence on positionCorrelation between speedclass and ejecta velocityHe/N novae are faster andbrighter than Fe iiFast novae more spatiallyextended than slow novae

1Shafter 2007, Shafter, Darnley,+ 2011, 2Shafter, Darnley,+ 2012, 3Shafter 2013Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 8 / 29

Multi-Wavelength Views and Correlations

Left: TLS Tautenburg — Right: Stiele+ 2011Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 9 / 29

Highlight: X-ray / Optical Correlations

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Henze+, 2014, A&A, 563, A2Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 10 / 29

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“Orange”: He/N — Blue: Fe ii

Henze+, 2014, A&A, 563, A2Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 11 / 29

Nova Parameter Space — Fujimoto/Nomoto Diagram

Kato+ 2014, ApJ, 793, 136; also see, e.g., Wolf+ 2013, ApJ, 777, 136Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 12 / 29

Recurrent Novae — the fast and the furious

> 1 observed eruption

Require: high MWD & Ṁ

Rapid evolution, high ejectavelocity, low ejected mass

Known systems:

Milky Way — 10SMC — 0LMC — 4 (or is it 5?)M 31 — 17

No (published) evidence ofNeon enhancement

Implication: all contain COWDs, all increasing in mass


The WD mass — growing or not — the He flashes

Net change in WD mass pereruption key to ultimate fate

Problem: He-flash ejects anyaccumulated material

Long term multi-cycleeruptions (e.g. Hillman+2014/15/16) may have solvedthe ‘problem’

Many authors: over longperiods, the WD mass grows(e.g., Hillman+, Starrfield+)


Recurrent Novae & Type Ia Supernovae

RNe are the most luminousSN Ia progenitor (candidate)

All quiescent novae with highṀ or giant donors can berecovered in the Local Group1

30%± 12% of M 31 novae havegiant donors1

25%± 10% of Galactic novaemay be RNe2

1/3 of all M 31 eruptions couldbe from RNe3

RNe unlikely to provide asignificant channel for theproduction of SN Ia3

1Williams, Darnley,+ 2016, 2Pagnotta & Schaefer 2014, 3Shafter, Henze,+ 2015Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 15 / 29

Rapidly Recurring Novae — a rapidly growing sample


M31N 2008-12a — Pushing the Boundaries

2008–2015: Recurrence period = 347± 10 days

Darnley, Henze,+ 2016, ApJ, 833, 149Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 17 / 29

M31N 2008-12a — Fast optical light curve

Darnley, Hounsell, Godon,+ 2017b, ApJ, 849, 96Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 18 / 29

M31N 2008-12a — He/N spectrum; decreasing velocities


M31N 2008-12a — brief and hot X-ray phase

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M31N 2008-12a — best SN Ia progenitor candidate

60% mass retention → WD growth toward Chandrasekhar massKato, Saio, Hachisu 2015, ApJ, 808, 52


M31N 2008-12a — Successful Pro-Am Collaboration


M31N 2008-12a — Delayed 2016 eruption

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Henze, Darnley,+ 2018, in prep.Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 23 / 29

M31N 2008-12a — Shortened SSS phase

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Henze, Darnley,+ 2018, ApJ, 857, 68Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 24 / 29

M31N 2008-12a — Disrupted Re-feeding?

Days after eruption

Henze, Darnley,+ 2018, ApJ, 857, 68Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 25 / 29

M31N 2008-12a — The Ultimate Fate

Prec = 347± 10 days1

MWD ' 1.38 M�(2) (no Ne(3))

Ṁ ∼ 10−6 M� yr−1 (1)

Donor — a red clump star1:

Ldonor = 103+12−11 L�

Rdonor = 14.1± 0.5 R�Teff,donor = 4900± 100 K

Porb & 5 days1

Low inclination – face-on?4

Detonation expected in< 20 kyr (1)

1Darnley+ 2017b, 2Henze+ 2018, 3Kato+ 2017, 4Darnley+ 2017a, 5Darnley+ 2016Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 26 / 29

M31N 2008-12a — The Ultimate Fate

Prec = 347± 10 days1

MWD ' 1.38 M�(2) (no Ne(3))Ṁ ∼ 10−6 M� yr−1 (1)

Donor — a red clump star1:

Ldonor = 103+12−11 L�

Rdonor = 14.1± 0.5 R�Teff,donor = 4900± 100 K

Porb & 5 days1

Low inclination – face-on?4

Detonation expected in< 20 kyr (1)

1Darnley+ 2017b, 2Henze+ 2018, 3Kato+ 2017, 4Darnley+ 2017a, 5Darnley+ 2016Darnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 26 / 29

M31N 2008-12a — A Nova Super-Remnant

M31N 2008-12a is surroundedby a vast, shell-like, nebula

HST imaging, ground-basedspectra & hydro simulationsindicate it is the remnant of upto 6 million eruptions of 12a1

During this period, theproposed CO WD has grownfrom its zero-age mass to theChandrasekhar mass

N

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1Darnley, Hounsell, O’Brien,+ submittedDarnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 27 / 29

M31N 2008-12a — A Nova Super-Remnant

M31N 2008-12a is surroundedby a vast, shell-like, nebula

HST imaging, ground-basedspectra & hydro simulationsindicate it is the remnant of upto 6 million eruptions of 12a1

During this period, theproposed CO WD has grownfrom its zero-age mass to theChandrasekhar mass

1Darnley, Hounsell, O’Brien,+ submittedDarnley & Henze (LJMU/SDSU) Novae in M31 — COSPAR 2018 July 19, 2018 27 / 29

The future of extragalactic nova science


History — One Hundred Years of Survey-tudeThree hundred's a crowd — Building Population StudiesMulti-Wavelength Views and CorrelationsInterface with Theoretical ModelsRecurrent Novae — The Fast and the FuriousM31N2008-12a — Pushing the BoundariesThe Future of Extragalactic Nova Science

Documents

Populations and properties of classical and recurrent novae in M31mjd/talks/COSPAR2018.pdf · 2019. 11. 8. · All quiescent novae with high M_ or giant donors can be recovered in