A New Review of Old Novae
Transcript of A New Review of Old Novae
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A New Review of Old Novae
Ashley Pagnotta
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Not necessarily quite this old…
Fontanille 2007
…but some are!
Judean coin depicting Nova 134 BC, also observed by Hipparchus.
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A New Review of Old Novae
What actually happensafter a nova eruption?
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A New Review of Old Novae
• Teruption + 0 years
• Teruption + 10 years• Teruption + 100 years
• Teruption + 1000 years
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A New Review of Old Novae
• Teruption + 0 years
• Teruption + 10 years• Teruption + 100 years
• Teruption + 1000 years
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First, the mass loss leads to an increase in theorbital separation of the two stars.
Shara et al. (1986)
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Second, sustained nuclear burning on the surface of the white dwarf irradiates & puff s up the companion.
Garlick/space-art.co.uk
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Is it a coincidence that these two eff ects cancel eachother out most of the time?
Collazzi et al. (2009)
Eruption
mpostmpre
Δm = mpre - mpost
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Is it a coincidence that these two eff ects cancel eachother out most of the time?
For CNe Exclusively:
• 25 systems
• 25 eruptions
• Δmavg = +0.16 mag
• Δmmed = +0.13 mag
• σ = 0.42 mag
Including RNe:
• 31 systems
• 44 eruptions
• Δmavg = +0.03 mag
• Δmmed = +0.03 mag
• σ = 0.43 mag
Collazzi et al. (2009)
Both consistent with Δm ≈ 0!
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But of course, there are a few weird systems thatrefuse to follow the rules.
Schaefer & Collazzi (2010)
Δm ≈ 4 mag
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But of course, there are a few weird systems thatrefuse to follow the rules.
Schaefer & Collazzi (2010)
Δm ≥ 5 mag
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The high Δm in the V1500 Cyg stars is thought tobe due to high magnetic fields in the systems.
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A New Review of Old Novae
• Teruption + 0 years
• Teruption + 10 years
• Teruption + 100 years
• Teruption + 1000 years
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• The hibernation theory was proposed to explain theabnormally low observed space density of novae.
• As the nuclear burning on the white dwarf turns off , theincrease in orbital separation dominates the system.
• The accretion rate slows and eventually turns off .
• There are (at least) two observable consequences of the
change in the accretion rate.
Shara et al. (1986)
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• The hibernation theory was proposed to explain theabnormally low observed space density of novae.
• As the nuclear burning on the white dwarf turns off , theincrease in orbital separation dominates the system.
• The accretion rate slows and eventually turns off .
• There are (at least) two observable consequences of the
change in the accretion rate.
Shara et al. (1986)
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• The hibernation theory was proposed to explain theabnormally low observed space density of novae.
• As the nuclear burning on the white dwarf turns off , theincrease in orbital separation dominates the system.
• The accretion rate slows and eventually turns off .
• There are (at least) two observable consequences of the
change in the accretion rate.
Shara et al. (1986)
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• The hibernation theory was proposed to explain theabnormally low observed space density of novae.
• As the nuclear burning on the white dwarf turns off , theincrease in orbital separation dominates the system.
• The accretion rate slows and eventually turns off .
• There are (at least) two observable consequences of the
change in the accretion rate.
Shara et al. (1986)
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As the accretion rate declines, the magnitude of thesystem must fade, eventually drastically.
Time
M a g n i t u d e
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As the accretion rate declines, the system will passthrough other CV classifications.
Nova
Nova-Like
DwarfNova
Hiberna2ng
DwarfNova
Nova-Like
N e t A c c r e t i onR
a t e D e c r e a s e s
N e t A c c r e t i o n R a t e I n c r e a s e s
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As the accretion rate declines, the magnitude of thesystem must fade, eventually drastically.
Time
M a g n i t u d e
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We can construct long term light curves of oldnovae to search for secular fading trends.
Neeley et al. (in prep)
For seven sources,average decline of 1.4 mag/century.
Decline = 1 mag/century
1933 2010
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Sometimes we also catch weird things, that don’tyet have a good theoretical explanation.
Schaefer (in prep)
14#
15#
16#
1870# 1890# 1910# 1930# 1950# 1970# 1990# 2010#
M a g n i t u d e
YEAR%
Q%CYG%(with%yearly%average%by%source%in%quiescence)%
Sonneberg#
AAVSO#Blue#
Shugarov#B#
Literature#Blue#
Asiago#
Harvard#
AAVSO#V#
Czech#
AFOEV#
Shugarov#V#
Steavenson#
Peek#
Barnard#
Literature#V#
Schmidt+#
Copeland#
Roboscope#
Eruption
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I am looking at a much larger sample to determinethe average behavior of post-nova systems.
321 Systems
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The Harvard College Observatory plate archive holdsmore than 500,000 plates dating to the 1890s.
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The Harvard College Observatory plate archive holdsmore than 500,000 plates dating to the 1890s.
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The DASCH Project, led by Josh Grindlay, isworking to scan all of the plates at CfA.
DASCH
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The DASCH Project, led by Josh Grindlay, isworking to scan all of the plates at CfA.
DASCH
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The DASCH Project, led by Josh Grindlay, isworking to scan all of the plates at CfA.
DASCH
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The DASCH Project, led by Josh Grindlay, isworking to scan all of the plates at CfA.
DR2 (b down to 60°) Coming October 1! DASCH
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One of the biggest challenges is actually locating thequiescent counterpart of the nova.
Downes & Shara Catalog
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Tappert, Ederoclite, Schmidtobreick, and Vogt areworking to identify old nova counterparts.
Tappert et al. (2012)
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We can monitor systems and watch as they transition fromone CV type to another, e.g. GK Per.
Shara et al. (2012)
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We can monitor systems and watch as they transition fromone CV type to another, e.g. GK Per.
Payne-Gaposchkin (1957)
JD - 2400000
M a g n i t u d
e
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V1017 Sgr has had many dwarf nova eruptions andone classical nova eruption since 1901.
1901 – Dwarf Nova
1919 – Classical Nova
1973 – Dwarf Nova
Webbink et al. (1987)
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A New Review of Old Novae
• Teruption + 0 years
• Teruption + 10 years
• Teruption + 100 years
• Teruption + 1000 years
7/27/2019 A New Review of Old Novae
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Z Cam was the first dwarf nova around which anancient classical nova shell was detected.
Shara et al. (2012)
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Z Cam is quite possibly associated with a guest starrecorded by Chinese astronomers in 77 BC.
Shara et al. (2012); Johansson (2007)
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AT Cancri is the second known dwarf nova with aconfirmed nova shell around it.
Shara et al. (2012)
1’
FUV NUV[NII]
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The AT Cancri shell looks very similar to that of GK Per & T Pyx, with Rayleigh-Taylor knots.
Toraskar et al. (2013)
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The spectrum of the AT Cancri shellconfirms that it is very bright in NII.
Shara et al. (2012)
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BK Lyn recently transitioned from nova-like to adwarf nova, and was likely a nova in 101 A.D.
Patterson et al. (2013)
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So it took BK Lyn 2000 years for DNe to begin, asopposed to ~50 years for GK Per—a Porb eff ect?
Patterson et al. (2013)
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CK Vul remains the most controversial old nova /eruptive stellar merger event.
Hajduk et al. (2013)
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Looking at a handful of systems gives mulitipleresults; a large-scale survey is crucial.
Time
M a g n i t u d e
Time
M a g n i t u d e
Time
M a g n i t u d e
e.g. V603 Aql
e.g. V1500 Cyg
e.g. Q Cyg
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A New Review of Old Novae
Post-nova systems:
• Fade
• Brighten
• Stay the Same
• Change States
• Quickly
• Slowly
• Are Exciting!