X-ray emission from novaeX-ray emission from novae
Glòria Sala
Univ. Politècnica de Catalunya (UPC)
Institut d'Estudis Espacials de Catalunya (IEEC)
OUTLINE
● Novae: What? Where? How? When? How many?
● As seen in the soft X-rays
● Recent and current observational programs
● As seen in the hard X-rays
X-ray emission from novaeX-ray emission from novae
NOVA OUTBURSTSWHAT?
Explosive Thermonuclear events in a white dwarf accreted envelope;
Ejection of fraction of envelope, enriched with nucleosynthetic products
NOVA OUTBURSTSWHAT?
Explosive Thermonuclear events in a white dwarf accreted envelope;
Ejection of fraction of envelope, enriched with nucleosynthetic products
SEE MORE AT JORDI JOSÉ'S
TALK ON WEDNESDAY
NOVA OUTBURSTSWHAT?
Explosive Thermonuclear events in a white dwarf accreted envelope;
Ejection of fraction of envelope, enriched with nucleosynthetic products
WHERE?
CATACLYSMIC VARIABLE(short orbital period, hours) White dwarf + dwarf star
accretion via Roche-Lobe overflow and accretion disk
SYMBIOTIC BINARY(long orbital periods, months-years)
White dwarf+ red giant or Mira accretion of red giant wind
Credit:Romano Corradi ant the IAC
Strong magnetic CV: polar
CATACLYSMIC VARIABLE (CV)
magnetic CV:
Intermediate polar
non-magnetic CV
NOVA OUTBURSTS
Credit:Romano Corradi ant the IAC
In Symbiotics,ejecta expands whithin
dense and complex giant wind
HOW?
In CVs: free balistic expansion,With internal or external (CSM) shocks
HOW MANY?
Total novae ~ 200Galactic rate ~30 novae/yr
(but just ~10 visible )
HOW OFTEN?
Classical novae (CNe): outburst every 105 years => obsserved once
Recurrent novae (RNe): outburst every few years/decades, more than one burst historically recorded
Nova outbursts in symbiotics are exotic.
9 Symbiotic novae(very long nova outburst,
evolving through years-decades)
4-5? Symbiotic recurrent novae known to date:
RS Oph, V745 Sco,
V3890 Sgr,T CrBand V407 Cyg ?
Credit:Romano Corradi ant the IAC
HOW MANY?
Total novae ~160 (up to year 2000)Galactic rate ~30 novae/yr (~10 seen)
HOW OFTEN?Classical novae (CNe):
every 105 years.
Recurrent novae (RNe):every a few years/decades, more than
one burst historically detected
RS Oph, V745 Sco,
V3890 Sgr,T CrBand V407 Cyg
Symbiotic recurrent novae
RNe occur on massive white dwarfs, close to Chandrasekhar mass
=> SNIa progenitor candidates!!
X-ray emission from classical novae
Super SOFT (photon energy <1 keV), “SSS”
- SOURCE: non-explosive H-burning in envelope left on the WD surface
- SPECTRUM: white dwarf atmosphere, kTeff ~30-50 eV (Teff ~2-10×105 K)
- LUMINOSITY: L~105 LSun
~ 1038 erg/s.
TRACES H-MASS LEFT ON WD SURFACE
Ejected materialEjected material
WD
ROSAT X-ray observations of V1974 Cyg (Krautter et al. 1996).
Rise due to decrease ofAbsorption => timescale related to ejected mass
Time (days)
X-r
ay f
lux
Soft X-ray emission due to residual H-burning
(black-body-like spectrum).
Soft X-ray emission due to residual H-burning
(black-body-like spectrum).
(Krautter et al. 1996).
Rise due to decrease ofabsorption
Energy (10 eV)
X-r
ay f
lux
Plateau, evolution path and duration related to white dwarf mass and envelope composition
Time (days)
X-r
ay f
lux
Soft X-ray emission due to residual H-burning
(black-body-like spectrum).
Final decay due to fuel exhaustion, related to envelope mass left on WD after outburst
Soft X-ray emission due to residual H-burning
(black-body-like spectrum). Nova Cyg 1992
(V1974 Cyg)
Comparison
of spectral evolution during
plateau and decay
with models
(Sala & Hernanz 2005a, A&A, 439, 1061)
provided limits on
white dwarf mass
(0.9-1.0 Msun)
(Sala & Hernanz 2005b A&A, 439, 1057)
XMM-Newton: observational follow-up of post-outburst Galactic novaeXMM-Newton: observational follow-up of post-outburst Galactic novaeXMM-Newton obsetvations between 2000-2007, PI: M. Hernanz
OBSERVATIONAL PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Target Discovery date
Date of observation – Time after outburst
Detection
N Sco 1997V1141 Sco
June 5 Oct. 11, 2000 – 1224d, 3.4yrMar. 24, 2001 – 1388d, 3.8yrSep. 7, 2001 – 1555d, 4.3yr
NO
N Sgr 1998V4633 Sgr
March 22 Oct. 11, 2000 – 934d, 2.6yrMar. 9, 2001 – 1083d, 3.0yrSep. 7, 2001 – 1265d, 3.5yr
YESbut no but no SSSSSS
N Oph 1998 V2487 Oph
June 15 Feb. 25, 2001 – 986d, 2.7 yrSep. 5, 2001 – 1178d, 3.2 yrFeb. 2002 – 1352d, 3.7yrSept. 24, 2002 – 1559d, 4.3yr
YESbut no but no SSSSSS
N Sco 1998V1142 Sco
October 21 Oct. 11, 2000 – 721 d, 2.0 yrMar. 24, 2001 – 885 d, 2.4 yrSep. 7, 2001 – 1052 d, 2.9 yr
2.62.6±±0.3 0.3 2.22.2±±0.4 0.4 1.21.2±±0.2 0.2
(10(10-2-2 cts/s) cts/s)
N Mus 1998LZ Mus
December 29
Dec. 28, 2000 – 730 d, 2.0 yrJun. 26, 2001 – 910 d, 2.5 yrDec. 26, 2001 – 1093 d 3.0 yr
NO?
• No supersoftNo supersoft X-ray emission related to residual H-burning detected X-ray emission related to residual H-burning detected all novae had already turned-offall novae had already turned-off • 3 out of 5 were emitting [thermal plasma (+ BB)] spectrum 3 out of 5 were emitting [thermal plasma (+ BB)] spectrum ejecta/accretion ejecta/accretion
XMM-Newton: observational follow-up of post-outburst Galactic novaeXMM-Newton: observational follow-up of post-outburst Galactic novae
OBSERVATIONAL PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Target Discovery date
Date of observation – Time after outburst
Detection
N Oph 1998 V2487 Oph
June 15 Mar. 24, 2007 – 8.8yrAO6 long exposure
YESbut no SSSbut no SSS
N Cyg 2005V2361 Cyg
February 10
May 13, 2006 - 15mo – bkg Oct. 20, 2006 - 20monthsAO5
--YES
marginal: (4.0marginal: (4.0±±0.8)x100.8)x10-3-3 cts/scts/s
N Sgr 2005aV5115 Sgr
March 28 Sep. 27, 2006 – 18monthsApr. 4, 2009 – 49 months
YES supersoft sourceYES but no SSS
N Sgr 2005bV5116 Sgr
July 4 Mar. 20, 2007 – 20 monthsMar. 13, 2009 – 44 months
YES supersoft sourceYES but no SSS
N Cyg 2006V2362 Cyg
April 2 May 5, 2007 – 13 monthsaffected by bkg AO6Dec. 22, 2008 – 32 months
YES but no SSS
YES but no SSS
N Oph 2006aV2575 Oph
February 9 Sep. 4, 2007 – 19 monthsAO6
NO
N Oph 2006bV2576 Oph
April 6 Oct. 3, 2007 – 18monthsAO6
NO
SupersoftSupersoft X-ray emission related to residual H-burning found in 2 novae from X-ray emission related to residual H-burning found in 2 novae from 2005 (V5115 Sgr & V5116 Sgr)2005 (V5115 Sgr & V5116 Sgr) novae had not turned-off yetnovae had not turned-off yet
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Swift: TOO triggered observations on Galactic
and Magellanic Cloud novae.
International collaboration, see www.swift.ac.uk/nova-cv/
Wolfgang Pietsch
Valerio Ribeiro
Mark Rushton
Gloria Sala (UPC-IEEC)
Brad Schaefer
Eric Schlegel
Greg Schwarz
Allen Shafter
Steve Shore
Gerry Skinner
Sumner Starrfield
Dai Takei
Gagik Tovmassian
Jim Truran
Neil Vaytet
R. Mark Wagner
Fred Walter
Pete Wheatley
Bob Williams
Graham Wynn
Andrew Helton
Arne Henden
Martin Henze (ESAC)
Margarida Hernanz (CSIC-IEEC)
Rebekah Hounsell
Aitor Ibarra (ESAC)
Jordi Jose (UPC-IEEC)
Amanpreet Kaur
Joachim Krautter
Erik Kuulkers (ESAC)
David Lynch
Elena Mason
Michael Philip Maxwell
Koji Mukai
Ulisse Munari
Jan-Uwe Ness (ESAC)
Tim O'Brien
Marina Orio
Kim Page
Ashley Pagnotta
Julian Osborne
Solen Balman
Andy Beardmore
Tomaso Belloni
Mike Bode
Laura Chomiuk
Matt Darnley
Ivan De Gennaro Aquino
Massimo Della Valle
Andrej Dobrotka
Jeremy Drake
Phil Evans
Stewart Eyres
Bob Gehrz
Ami Glasner
Rosario Gonzalez (ESAC)
Jochen Greiner
Daniel Harman
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Swift: TOO triggered observations on Galactic
and Magellanic Cloud novae.
RS Oph, outburst in 2006
(Osborne et al 2011, ApJ 727, 124)
RS Oph, outburst in 2006
(Osborne et al 2011, ApJ 727, 124)
V2491 Cyg
(Page et al 2010 A&A 507, 923)
International collaboration, see www.swift.ac.uk/nova-cv/
Good monitoring and follow-up of the SSS phase, both in X-ray and UV
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Martin Henze
Novae in M31: monitoring program with XMM-Newton, Chandra and Swift.
LARGER STATISTICS THAN IN THE GALAXY, 1-2 OPTICAL NOVAE PER MONTH
EASY MONITORING OF SSS IN CENTRAL AREA,COVERED WITH EPIC FOV AND LOW ABSOPRTION => 79 SSS NOVAE UP TO NOW!
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Novae in M31: monitoring program with XMM-Newton, Chandra and Swift.
FIRST RELATIONS BETWEEN X-RAY AND OPTICAL PARAMETERS AVAILABLE,
Henze et al. 2011, A&A, 533, A52
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Novae in M31: monitoring program with XMM-Newton, Chandra and Swift.
(lead by Wolfgang Pietsch, MPE; Martin Henze, ESAC)
see www.mpe.mpg.de/~m31novae/)
Papers from this work:
“Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126”Henze, M.; Pietsch, W.; Haberl, F.; Della Valle, M.; Riffeser, A.; Sala, G.; Hatzidimitriou, D. et al. 2013, A&A, 549, A120
“M31N 2008-05d: a M 31 disk nova with a dipping supersoft X-ray light curve”Henze, M.; Pietsch, W.; Haberl, F.; Hernanz, M.; Sala, G.; Della Valle, M.; Stiele, H. 2012, A&A, 544, A44
“X-ray monitoring of classical novae in the central region of M 31, II. Autumn and winter 2007/2008 and 2008/2009”Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Hatzidimitriou, D., Della Valle, M., Rau, A., Hartmann, D.H., Burvitz, V.2011, A&A, 533, A52
Nova M31N 2007-12b: supersoft X-rays reveal an intermediate polar?Pietsch, W., Henze, M., Haberl, F., Hernanz, M., Sala, G., Hartmann, D.H., Della Valle, M.2011, A&A, 531, A22
X-ray monitoring of classical novae in the central region of M 31, I. June 2006 - March 2007Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Della Valle, M., Hatzidimitriou, D., Rau, A., Hartmann, D.H., Greiner, J., Burvitz, V., Fliri, J.2010, A&A, 523, A89
The very short supersoft X-ray state of the classical nova M31N 2007-11aHenze, M., Pietsch, W., Sala, G., Della Valle, M., Hernanz, M., Greiner, J., Burwitz, V., Freyberg, M.J., Haberl F., Hartmann, D.H., Milne, P., Williams, G.G.2009, A&A, 498, L13
The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novaeHenze, M., Pietsch, W., Haberl F., Sala, G., Quimby, R., Hernanz, M., Della Valle, M., Milne, P., Williams, G.G., Burwitz, V., Greiner, J., Stiele, H., Hartmann, D.H., Kong, A.K.H., Hornoch, K.2009, A&A, 500, 769
X-ray monitoring of optical novae in M31 from July 2004 to February 2005Pietsch, W., Haberl, F., Sala, G., Stiele, H., Hornoch, K., Riffeser, A., Fliri, J., Bender, R., Buehler, S., Burwitz, V., Greiner, J., Seitz, S. 2007, A&A, 465, 375
Optical novae: the major class of supersoft X-ray sources in M 31Pietsch, W., Fliri, J., Freyberg, M. J., Greiner, J., Haberl, F., Riffeser, A., Sala, G.2005, A&A, 442, 879
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Novae in M31: monitoring program with XMM-Newton, Chandra and Swift.
(lead by Wolfgang Pietsch, MPE; Martin Henze, ESAC)
see www.mpe.mpg.de/~m31novae/)
MONITORING PAPERS“Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126”Henze, M.; Pietsch, W.; Haberl, F.; Della Valle, M.; Riffeser, A.; Sala, G.; Hatzidimitriou, D. et al. 2013, A&A, 549, A120
“M31N 2008-05d: a M 31 disk nova with a dipping supersoft X-ray light curve”Henze, M.; Pietsch, W.; Haberl, F.; Hernanz, M.; Sala, G.; Della Valle, M.; Stiele, H. 2012, A&A, 544, A44
“X-ray monitoring of classical novae in the central region of M 31, II. Autumn and winter 2007/2008 and 2008/2009”Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Hatzidimitriou, D., Della Valle, M., Rau, A., Hartmann, D.H., Burvitz, V.2011, A&A, 533, A52
Nova M31N 2007-12b: supersoft X-rays reveal an intermediate polar?Pietsch, W., Henze, M., Haberl, F., Hernanz, M., Sala, G., Hartmann, D.H., Della Valle, M.2011, A&A, 531, A22
X-ray monitoring of classical novae in the central region of M 31, I. June 2006 - March 2007Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Della Valle, M., Hatzidimitriou, D., Rau, A., Hartmann, D.H., Greiner, J., Burvitz, V., Fliri, J.2010, A&A, 523, A89
The very short supersoft X-ray state of the classical nova M31N 2007-11aHenze, M., Pietsch, W., Sala, G., Della Valle, M., Hernanz, M., Greiner, J., Burwitz, V., Freyberg, M.J., Haberl F., Hartmann, D.H., Milne, P., Williams, G.G.2009, A&A, 498, L13
The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novaeHenze, M., Pietsch, W., Haberl F., Sala, G., Quimby, R., Hernanz, M., Della Valle, M., Milne, P., Williams, G.G., Burwitz, V., Greiner, J., Stiele, H., Hartmann, D.H., Kong, A.K.H., Hornoch, K.2009, A&A, 500, 769
X-ray monitoring of optical novae in M31 from July 2004 to February 2005Pietsch, W., Haberl, F., Sala, G., Stiele, H., Hornoch, K., Riffeser, A., Fliri, J., Bender, R., Buehler, S., Burwitz, V., Greiner, J., Seitz, S. 2007, A&A, 465, 375
Optical novae: the major class of supersoft X-ray sources in M 31Pietsch, W., Fliri, J., Freyberg, M. J., Greiner, J., Haberl, F., Riffeser, A., Sala, G.2005, A&A, 442, 879
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Novae in M31: monitoring program with XMM-Newton, Chandra and Swift.
(lead by Wolfgang Pietsch, MPE; Martin Henze, ESAC)
see www.mpe.mpg.de/~m31novae/)
EXTRAORDINARY SSS NOVAE: SSS and NOVAE in GLOBULAR CLUSTERS
“Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126”Henze, M.; Pietsch, W.; Haberl, F.; Della Valle, M.; Riffeser, A.; Sala, G.; Hatzidimitriou, D. et al. 2013, A&A, 549, A120
“M31N 2008-05d: a M 31 disk nova with a dipping supersoft X-ray light curve”Henze, M.; Pietsch, W.; Haberl, F.; Hernanz, M.; Sala, G.; Della Valle, M.; Stiele, H. 2012, A&A, 544, A44“X-ray monitoring of classical novae in the central region of M 31, II. Autumn and winter 2007/2008 and 2008/2009”Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Hatzidimitriou, D., Della Valle, M., Rau, A., Hartmann, D.H., Burvitz, V.2011, A&A, 533, A52
Nova M31N 2007-12b: supersoft X-rays reveal an intermediate polar?Pietsch, W., Henze, M., Haberl, F., Hernanz, M., Sala, G., Hartmann, D.H., Della Valle, M.2011, A&A, 531, A22
X-ray monitoring of classical novae in the central region of M 31, I. June 2006 - March 2007Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Della Valle, M., Hatzidimitriou, D., Rau, A., Hartmann, D.H., Greiner, J., Burvitz, V., Fliri, J.2010, A&A, 523, A89
The very short supersoft X-ray state of the classical nova M31N 2007-11aHenze, M., Pietsch, W., Sala, G., Della Valle, M., Hernanz, M., Greiner, J., Burwitz, V., Freyberg, M.J., Haberl F., Hartmann, D.H., Milne, P., Williams, G.G.2009, A&A, 498, L13
The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novaeHenze, M., Pietsch, W., Haberl F., Sala, G., Quimby, R., Hernanz, M., Della Valle, M., Milne, P., Williams, G.G., Burwitz, V., Greiner, J., Stiele, H., Hartmann, D.H., Kong, A.K.H., Hornoch, K.2009, A&A, 500, 769
X-ray monitoring of optical novae in M31 from July 2004 to February 2005Pietsch, W., Haberl, F., Sala, G., Stiele, H., Hornoch, K., Riffeser, A., Fliri, J., Bender, R., Buehler, S., Burwitz, V., Greiner, J., Seitz, S. 2007, A&A, 465, 375
Optical novae: the major class of supersoft X-ray sources in M 31Pietsch, W., Fliri, J., Freyberg, M. J., Greiner, J., Haberl, F., Riffeser, A., Sala, G.2005, A&A, 442, 879
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Novae in M31: monitoring program with XMM-Newton, Chandra and Swift.
(lead by Wolfgang Pietsch, MPE; Martin Henze, ESAC)
see www.mpe.mpg.de/~m31novae/)
EXTRAORDINARY SSS NOVAE: SSS and NOVAE in GLOBULAR CLUSTERS
“Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126”Henze, M.; Pietsch, W.; Haberl, F.; Della Valle, M.; Riffeser, A.; Sala, G.; Hatzidimitriou, D. et al. 2013, A&A, 549, A120
“M31N 2008-05d: a M 31 disk nova with a dipping supersoft X-ray light curve”Henze, M.; Pietsch, W.; Haberl, F.; Hernanz, M.; Sala, G.; Della Valle, M.; Stiele, H. 2012, A&A, 544, A44“X-ray monitoring of classical novae in the central region of M 31, II. Autumn and winter 2007/2008 and 2008/2009”Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Hatzidimitriou, D., Della Valle, M., Rau, A., Hartmann, D.H., Burvitz, V.2011, A&A, 533, A52
Nova M31N 2007-12b: supersoft X-rays reveal an intermediate polar?Pietsch, W., Henze, M., Haberl, F., Hernanz, M., Sala, G., Hartmann, D.H., Della Valle, M.2011, A&A, 531, A22
X-ray monitoring of classical novae in the central region of M 31, I. June 2006 - March 2007Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Della Valle, M., Hatzidimitriou, D., Rau, A., Hartmann, D.H., Greiner, J., Burvitz, V., Fliri, J.2010, A&A, 523, A89
The very short supersoft X-ray state of the classical nova M31N 2007-11aHenze, M., Pietsch, W., Sala, G., Della Valle, M., Hernanz, M., Greiner, J., Burwitz, V., Freyberg, M.J., Haberl F., Hartmann, D.H., Milne, P., Williams, G.G.2009, A&A, 498, L13
The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novaeHenze, M., Pietsch, W., Haberl F., Sala, G., Quimby, R., Hernanz, M., Della Valle, M., Milne, P., Williams, G.G., Burwitz, V., Greiner, J., Stiele, H., Hartmann, D.H., Kong, A.K.H., Hornoch, K.2009, A&A, 500, 769
X-ray monitoring of optical novae in M31 from July 2004 to February 2005Pietsch, W., Haberl, F., Sala, G., Stiele, H., Hornoch, K., Riffeser, A., Fliri, J., Bender, R., Buehler, S., Burwitz, V., Greiner, J., Seitz, S. 2007, A&A, 465, 375
Optical novae: the major class of supersoft X-ray sources in M 31Pietsch, W., Fliri, J., Freyberg, M. J., Greiner, J., Haberl, F., Riffeser, A., Sala, G.2005, A&A, 442, 879
All three novae in M31 GCs are hot and fast => massive WD!
MONITORING PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Novae in M31: monitoring program with XMM-Newton, Chandra and Swift.
(lead by Wolfgang Pietsch, MPE; Martin Henze, ESAC)
see www.mpe.mpg.de/~m31novae/)
EXTRAORDINARY SSS NOVAE: VARIABLE SSS LIGHT-CURVES“Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126”Henze, M.; Pietsch, W.; Haberl, F.; Della Valle, M.; Riffeser, A.; Sala, G.; Hatzidimitriou, D. et al. 2013, A&A, 549, A120
“M31N 2008-05d: a M 31 disk nova with a dipping supersoft X-ray light curve”Henze, M.; Pietsch, W.; Haberl, F.; Hernanz, M.; Sala, G.; Della Valle, M.; Stiele, H. 2012, A&A, 544, A44“X-ray monitoring of classical novae in the central region of M 31, II. Autumn and winter 2007/2008 and 2008/2009”Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Hatzidimitriou, D., Della Valle, M., Rau, A., Hartmann, D.H., Burvitz, V.2011, A&A, 533, A52
Nova M31N 2007-12b: supersoft X-rays reveal an intermediate polar?Pietsch, W., Henze, M., Haberl, F., Hernanz, M., Sala, G., Hartmann, D.H., Della Valle, M.2011, A&A, 531, A22
X-ray monitoring of classical novae in the central region of M 31, I. June 2006 - March 2007Henze, M., Pietsch, W., Haberl, F., Hernanz, M., Sala, G., Della Valle, M., Hatzidimitriou, D., Rau, A., Hartmann, D.H., Greiner, J., Burvitz, V., Fliri, J.2010, A&A, 523, A89
The very short supersoft X-ray state of the classical nova M31N 2007-11aHenze, M., Pietsch, W., Sala, G., Della Valle, M., Hernanz, M., Greiner, J., Burwitz, V., Freyberg, M.J., Haberl F., Hartmann, D.H., Milne, P., Williams, G.G.2009, A&A, 498, L13
The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novaeHenze, M., Pietsch, W., Haberl F., Sala, G., Quimby, R., Hernanz, M., Della Valle, M., Milne, P., Williams, G.G., Burwitz, V., Greiner, J., Stiele, H., Hartmann, D.H., Kong, A.K.H., Hornoch, K.2009, A&A, 500, 769
X-ray monitoring of optical novae in M31 from July 2004 to February 2005Pietsch, W., Haberl, F., Sala, G., Stiele, H., Hornoch, K., Riffeser, A., Fliri, J., Bender, R., Buehler, S., Burwitz, V., Greiner, J., Seitz, S. 2007, A&A, 465, 375
Optical novae: the major class of supersoft X-ray sources in M 31Pietsch, W., Fliri, J., Freyberg, M. J., Greiner, J., Haberl, F., Riffeser, A., Sala, G.2005, A&A, 442, 879
(Pietsch et al. 2011, A&A 531, 22)
Soft X-ray => Nova M31N 2007-12b: an intermediate polar?
20-60 days after outburstVARIABILITY in the SSS!!
Stable 1100 s period (WD spin)Dips suggest 4.9 or 9.8 hr orbit
Sala, Hernanz, Ferri, Greiner, ApJ 675, L93 (2008)
VARIABILITY in the SSS!!Orbital period: occultation of
the central WD during 2/3 of orbitAsymmetric disk?
OPEN PROBLEMS 1:
variability in the SSS emission: dips, flares and periodicities
V5116 Sgr
Soft X-ray => H-burning
The symbiotic recurrent nova
RS Oph (2006 outburst)
SSS emission as seen by Swift
VARIABILITY in the SSS!!Transient 35 s modulation;fusion driven instability?(Osborne et al 2006, 2011)
RS Oph
variability in the SSS emission
Soft X-ray emission due to residual H-burning
V1494 Aql: 2500s peaks
(non-radial g+ modes of WD)
(Drake et al 2003)
RS Oph: transient 35 s modulation
fusion instability?
(Osborne 2006, Ness 2007)
V4743 Sgr: 1330 s periodicity (WD spin?)
And long dip
(Dobrotka & Ness 2010)
V5116 Sgr: orbital period, 3.2 hrs,
(Sala et al 2008)
M31N 2007-12b: IP-like,
WD spin and orbital period?
(Pietsch et al. 2011)
V2491 Cyg:
37min period and a dip
WD spin??
(Ness et al 2011)
V2491Cyg: RGS spectra. Good NLTE models of expanding atmospheres still missing
(Ness et al. ApJ, 733, 70)
OPEN PROBLEMS 2:
white dwarf atmosphere spectral models
V2491Cyg: RGS spectra. Good NLTE models of expanding atmospheres still missing
(Ness et al. ApJ, 733, 70)
OPEN PROBLEMS 2:
white dwarf atmosphere spectral models
SEE MORE AT JAN-UWE NESS'S
TALK ON WEDNESDAY
X-ray emission from classical novae
1. Super SOFT (photon energy <1 keV), “SSS”
TRACES H-MASS LEFT ON WD SURFACE
Ejected materialEjected material
WD
2. Ejecta's HARD (photon energy 1-50 keV)
- SOURCE: shocks in ejecta or from ejecta with CSM
- SPECTRUM: thermal plasma, highly ionized species
- LUMINOSITY: L~1033-34 erg/s.
TRACES EJECTA AND CSM
- In Symbiotic systems => shocks with red
giant wind => strong hard X-rays and particle acceleration
3. Accretion's HARD (photon energy 1-50 keV), “CV like”
- SOURCE: hot accretion disk reestablished
- SPECTRUM: Thermal bremsstrahlung, Fe I
- LUMINOSITY: L~1033-34 erg/s.TRACES ACCRETION FLOW
XMM-Newton: observational follow-up of post-outburst Galactic novaeXMM-Newton: observational follow-up of post-outburst Galactic novaeXMM-Newton obsetvations between 2000-2007, PI: M. Hernanz
OBSERVATIONAL PROGRAMS AIMED TO CATCH THE SSS EMISSION OF NOVAE :
Target Discovery date
Date of observation – Time after outburst
Detection
N Sco 1997V1141 Sco
June 5 Oct. 11, 2000 – 1224d, 3.4yrMar. 24, 2001 – 1388d, 3.8yrSep. 7, 2001 – 1555d, 4.3yr
NO
N Sgr 1998V4633 Sgr
March 22 Oct. 11, 2000 – 934d, 2.6yrMar. 9, 2001 – 1083d, 3.0yrSep. 7, 2001 – 1265d, 3.5yr
YESbut no but no SSSSSS
N Oph 1998 V2487 Oph
June 15 Feb. 25, 2001 – 986d, 2.7 yrSep. 5, 2001 – 1178d, 3.2 yrFeb. 2002 – 1352d, 3.7yrSept. 24, 2002 – 1559d, 4.3yr
YESbut no but no SSSSSS
N Sco 1998V1142 Sco
October 21 Oct. 11, 2000 – 721 d, 2.0 yrMar. 24, 2001 – 885 d, 2.4 yrSep. 7, 2001 – 1052 d, 2.9 yr
2.62.6±±0.3 0.3 2.22.2±±0.4 0.4 1.21.2±±0.2 0.2
(10(10-2-2 cts/s) cts/s)
N Mus 1998LZ Mus
December 29
Dec. 28, 2000 – 730 d, 2.0 yrJun. 26, 2001 – 910 d, 2.5 yrDec. 26, 2001 – 1093 d 3.0 yr
NO?
• No supersoftNo supersoft X-ray emission related to residual H-burning detected X-ray emission related to residual H-burning detected all novae had already turned-offall novae had already turned-off • 3 out of 5 were emitting [thermal plasma (+ BB)] spectrum 3 out of 5 were emitting [thermal plasma (+ BB)] spectrum ejecta/accretion ejecta/accretion
Glòria Sala (GAA, FEN UPC)19 de Novembre de 2008, EUETIB
Nova Sgr 1998(V4633 Sgr)
Hard X-ray emission associated to the ejected material
(Hernanz & Sala 2007, The Astrophysical Journal, 664, 467)
2. Hard X-ray emission due to schocked shell
(thermal bremsstrahlung spectrum)
WD
kT1
kT2 kT
3
XMM-Newton, EPIC unfolded spectra
XMM-Newton: observational follow-up of post-outburst Galactic novaeXMM-Newton: observational follow-up of post-outburst Galactic novae
XMM-Newton: observational follow-up of post-outburst Galactic novaeXMM-Newton: observational follow-up of post-outburst Galactic novae
Nova Oph 1998(V2487 Oph)Hard X-ray emission,
2T Thermal plasma (kT1~ 0.22 keV, kT2 >
48 keV) + Gaussian line E = 6.4 keV
Fluorescence FeKα line,signature of accretion
disc, reestablished less than 1000 days after the nova explosion
Also detected by ROSAT during RASS in 1990!!
(Hernanz & Sala 2002, Science 664, 467)
Low THigh T
Fe Kα
3. Hard X-rays due to accretion disk (thermal bremsstrahlung spectrum)
XMM-Newton, EPIC spectra and best-fit model
Prompt (day 9) superhard (up to 70 keV) and later (days 29-150) hard X-rays
V2491 Cyg as seen by XMM, Suzaku and Swift
Takei et al 2009, ApJL: prompt superhard X-rays
Takei et al. 2011 PASJ: X-ray study of rekindled accretion...
X-ray emission from classical novae
1. Super SOFT (photon energy <1 keV), “SSS”
2. Ejecta's HARD (photon energy 1-50 keV)
- SOURCE: shocks in ejecta or from ejecta with CSM
- SPECTRUM: thermal plasma, highly ionized species
- LUMINOSITY: L~1033-36 erg/s.
TRACES EARLY EJECTA
PROPERTIES AND CSM
3. Accretion's HARD (photon energy 1-50 keV), “CV like”
- SOURCE: hot accretion disk reestablished
- SPECTRUM: Thermal bremsstrahlung, Fe I
- LUMINOSITY: L~1033-34 erg/s.TRACES ACCRETION FLOW
BUT TIMING IN THE HARD BAND NOT TESTED AS IN THE sss
BECAUSE OF LOW/BAD STATISTICS
LOFT CAN DO IT!!!
Ejected materialEjected material
WD
Day LAD (10 ks) cts/s WFM (1ks) cts/s
3 3.8x104 (+/-2) 46 (+/-1)
6 2.6x104 (+/-2) 30 (+/-1)
10 1.1x104 (+/-2) 13 (+/-1)
1 ks
Symbiotic Recurrent Novae:Trigger WFM early in outburst
WFM
LAD
For all novae:Probing nova ejection and accretion:Timing of Fe lines probe origin site, ejecta, accretion flow, reflection...
RS Oph simulations
RS Oph inWFM
RS Oph in LAD,10 ks
RS Oph In RXTE/PCA
Fe lines ofV2491 Cyg in LAD,10 ks
LOFT: Large Observatory For Timing in X-rays
Day LAD (10 ks) cts/s WFM (1ks) cts/s
3 3.8x10 4 (+/-2) 46 (+/-1)
6 2.6x10 4 (+/-2) 30 (+/-1)
10 1.1x10 4 (+/-2) 13 (+/-1)
1 ks
Symbiotic Recurrent Novae:Trigger WFM early in outburst
WFM
LAD
For all novae:Probing nova ejection and accretion:Timing of Fe lines probe origin site, ejecta, accretion flow, reflection...
RS Oph simulations
RS Oph inWFM
RS Oph in LAD,10 ks
RS Oph In RXTE/PCA
Fe lines ofV2491 Cyg in LAD,10 ks
LOFT: Large Observatory For Timing in X-rays
SEE MORE ON LOFT AT MARGARITA HERNANZ'S
TALK AFTER THE COFFEE BREAK
Higher energy emission from novae in symbioticsAbdo et al. 2010, Science
π0 decay produces gamma rays,
π0 originated in shock front of ejecta with red giant wind =>RSOph-like!
NOW TWO MORE RECENT FERMIDETECTIONS OF NOVAE:
Nova Mon 2012(Cheung et al. ATel #4284)Nova Sco 2012 (Cheung et al. ATel #4310)
Tatischeff & Hernanz (2007ApJ) predicted gammas for RS Oph, but no Fermi to see them in 2006!
Summary and conclusions
● Soft X-rays from novae trace envelope left on WD
● Good monitoring programs plus pointed observations arise new questions: Variability? Expanding atmospheres?
● Hard X-rays from novae probe ejection and accretion
● LOFT opens a new window in the timing studies of nova ejecta => time resolved Fe lines spectroscopy would probe emission site (ejecta, disk, reflection)
● Shocks of ejecta with red giant wind in Symbiotic-like Recurrent Novae (like RS Oph) produce very bright prompt hard X-ray emission => trigger in WFM in LOFT
Summary and conclusions
● Soft X-rays from novae trace envelope left on WD
● Good monitoring programs plus pointed observations arise new questions: Variability? Expanding atmospheres?
● Hard X-rays from novae probe ejection and accretion
● LOFT opens a new window in the timing studies of nova ejecta => time resolved Fe lines spectroscopy would probe emission site (ejecta, disk, reflection)
● Shocks of ejecta with red giant wind in Symbiotic-like Recurrent Novae (like RS Oph) produce very bright prompt hard X-ray emission => trigger in WFM in LOFT
SEE MORE ON NOVAE ON WEDNESDAY