recurrent nova t pyx: a normal nova eruption ~1866 shell ejected in 1866±5 v expansion for shell is...
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RECURRENT NOVA T Pyx:A NORMAL NOVA ERUPTION ~1866
Shell ejected in 1866±5
Vexpansion for shell is 500-715 km/sMshell is 10-4.5 M
}ClassicalNova Eruption In 1866
1994
2007
MWD dominated by ejections of regular nova events, so is losing mass
Short-Porb recurrent novae are not SN progenitors
GET Mejecta FROM PERIOD CHANGE ACROSS ERUPTIONS
Mejecta = (MWD/A)*(P/P)
U SCO 2010 ERUPTION:LARGE PERIOD CHANGE
2452000-0.010
-0.005
0.000
0.005
0.010
0.015
0.020
U SCO
Julian Date
O-C
(d
ays) 2
010 E
rupti
on
• P = (27.6 ± 1.4) x 10-6 days• Mejecta = (27.7 ± 1.4) x 10-6 M
• T = 10.9 years, M = (0.1±0.05) x 10-6 M/yr
T PYX 2011 ERUPTION:LARGE PERIOD CHANGE
• P = (4.0 ± 0.3) x 10-6 days• Mejecta = (58.8 ± 5.5) x 10-6 M
• T = 44.3 years, M = (0.1±0.05) x 10-6 M/yr
2454400 2454800 2455200 2455600 2456000 2456400-0.005
0.000
0.005
0.010
0.015
0.020
0.025
0.030
0.035
0.040
T Pyx
Julian Date
O-C
(d
ays)
Sta
rt o
f 2011 E
rupti
on
CI AQL 2000 ERUPTION:SUBSTANTIAL PERIOD CHANGE
• P = (1.5 ± 1.0) x 10-6 days• Mejecta = (2.9 ± 2.0) x 10-6 M
• T = 24 years, M = (0.1±0.05) x 10-6 M/yr
2448000 2449000 2450000 2451000 2452000 2453000 2454000 2455000 2456000-0.020
-0.015
-0.010
-0.005
0.000
0.005
0.010
0.015
CI Aql
Julian Date
O-C
(d
ays)
2000 E
rupti
on
RECURRENT NOVA WHITE DWARFS ARE EJECTING MORE MASS THAN THEY ARE ACCRETING
RNe Year Mejecta(10-
6M)MDT(10-
6M)Mejecta/MDT
U Sco 2010 27.7±1.4 1.1 25
T Pyx 2011 58.8±5.5 4.4 13
CI Aql 2000 2.9±2.0 2.4 1.2
RNe WDs losing massRNe will not become Type Ia
supernova
HALF OF THE RECURRENT NOVAE ARE NEON NOVAE
Half-or-more of RN will not become supernovae
A neon nova cannot have its WD gaining mass, because it is dredging up new material each eruption.
A neon nova must have an underlying ONeMg WD and cannot become a supernova, because it is not the required CO white dwarf.
NEON NOVAE
U Sco
RS Oph
YY Dor
Nova LMC 2009
FeII NOVAE
T CrB
V394 CrA
V3890 Sgr
IM Nor
Mason et al. 2012, A&A
RN SUMMARY SO FAR:T Pyx MS companion
✖WD is losing mass
IM Nor MS companion
✖CN eruption means WD is losing mass
V2487 Oph
Subgiant companion
U Sco Subgiant companion
✖ONeMg WD, WD losing mass
CI Aql Subgiant companion
✖WD is losing mass
V394 CrA Subgiant companion
T CrB Red Giant companion
RS Oph Red Giant companion ✖ONeMg WD
V745 Sco Red Giant companion
V3890 Sgr
Red Giant companion
THE COMPANION STAR CAN DISTINGUISH THE PROGENITOR
DoubleDegenerate
Recurrent Novae
Symbiotic Stars
HeliumStars
PersistentSupersoftSources
Pre-eruption companion to WD
WD Red Giant,Subgiant,MS
Red Giant Hi-Lum. star ‘core’
Subgiant,>1.2M MS
Post-eruption ex-companion
...none... Red Giant,Subgiant,MS
Red Giant Hi-Lum. star ‘core’
Subgiant,>1.2M MS
3-s error circle:Measurement Error
+Orbital Velocity
+Kicks
SNR 0509-67.5 FINAL 3-s ERROR CIRCLEIS EMPTY OF POINT SOURCES TO V=26.9
THE UTTER LACK OF ANY EX-COMPANION RULES OUT ALL MODELS
EXCEPT THE DOUBLE DEGENERATE
Schaefer & Pagnotta 2012, Nature
Limiting mag of V=26.9 MV=8.4 (K9 on main sequence)
✖ ✖✖ ✖DoubleDegenerate
Recurrent Novae
Symbiotic Stars
HeliumStars
PersistentSupersoftSources
Post-eruption ex-companion
...none... Red Giant,Subgiant,MS
Red Giant Hi-Lum. star ‘core’
Subgiant,>1.2M MS
TWO MORE LMC TYPE Ia SN REMNANTS HAVE NO RED GIANT or SUBGIANT EX-COMPANIONS
SNR 0505-67.9SNR 0519-69.0
Edwards, Pagnotta, & Schaefer 2012, ApJLett
SN1006 HAS NO RED GIANT EX-COMPANION
Gonzalez-Hernandez et al. 2012, Nature
Li et al. (2011) (arXiv)
SN 2011fe HAS NO RED GIANT COMPANIONLi et al. 2011, Nature
Lack of any counterpart on pre-eruption HST images proves the companion cannot be a luminous red giant or a luminous Helium star.
NO ‘KASEN EFFECT’ IN 235 SUPERNOVAE MEANS NO RED GIANT COMPANION
Kasen 2010, ApJ
Supernova Survey # supernova
# with Kasen effect
SDSSHayden et al. 2010,ApJ
108 0
SNLSBianco et al. 2011,ApJ
100 0
LOSSGaneshalingam et al. 2010,ApJ
61 0
NO EMISSION FROM EJECTA/WIND COLLISION MEANS NO RED GIANT COMPANION
Wavelength Instrument # supernova
# with emission
X-ray SwiftRussell & Immler 2012,ApJLett
53 0
Ultraviolet
SwiftBrown et al. 2012,ApJ
12 0
Radio VLAHancock et al. 2011,ApJ
46 0
Radio EVLAChomiuk et al. 2012,ApJ
1 (SN2011fe) 0
BUT:A few SNe (PTF11kx, SN2002ic, & SN2005gj) show variable narrow emission lines that are a clear hall mark of interaction with a circumstellar medium 0.1% - 1% of progenitors are Symbiotic Stars
SCORECARD FOR RED GIANT COMPANIONS:# Supernova Examined
# with Red Giants
SNR 0509-67.5 1 0
2 LMC SNRs 2 0
Tycho’s & SN1006 2 0
SN 2011fe 1 0
No Kasen Effect 269x10% 0
No Wind/Ejecta Collision
112 0
_____ ___145 0
RN SUMMARY:T Pyx MS companion ✖WD is losing mass
IM Nor MS companion ✖CN eruption means WD is losing mass
V2487 Oph
Subgiant companion ✖No subgiant companions
U Sco Subgiant companion ✖ONeMg WD, WD losing mass
CI Aql Subgiant companion ✖WD is losing mass
V394 CrA Subgiant companion ✖No subgiant companions
T CrB Red Giant companion ✖No red giant companions
RS Oph Red Giant companion ✖ONeMg WD
V745 Sco Red Giant companion ✖No red giant companions
V3890 Sgr
Red Giant companion ✖No red giant companions
GENERALIZING –IF ONE CLASS DOMINATEs:
DoubleDegenerate
Recurrent Novae
Symbiotic Stars
HeliumStars
PersistentSupersoftSources
First Progenitor Class ✓✖✖✖✖
No RedGiants
No RedGiants
SNR0509center is empty
Neon WDs,
Mejecta too high
SNR0509center is empty
No Hi-Lstars
No Kasen effect
GENERALIZING –IF TWO CLASSES DOMINATE:
DoubleDegenerate
Recurrent Novae
Symbiotic Stars
HeliumStars
PersistentSupersoftSources
First Progenitor Class ✓✖✖✖✖SecondProgenitor Class ??? ✖✖✖✖ ?
No Kasen effect
Different from first class
No RedGiants
No RedGiants
SNR0509center is empty
No RedGiants
No RedGiants
Neon WDs,
Mejecta too high
SNR0509center is empty
Neon WDs,
Mejecta too high
No Hi-Lstars
No Hi-Lstars
No Kasen effect
CONCLUSIONS:
or
SUPERSOFT? DOUBLE DEGENERATE
SYM
BIO
TIC
DOUBLE DEGENERATE
SYM
BIO
TIC
Two RNe have Mejecta>>MDT
Half of the RNe are neon nova
T Pyx had a classical nova eruption in 1866 and is fast exiting the RN phase
SNR0509-67.5 has an empty central region to MV= +8.4
Out of a sample of 145 SNe, 0 have red giant companions(with similar but weaker restrictions for subgiant companions)