Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz1 Grains and Gas in the Ejecta of Classical Novae R. D. Gehrz Department of Astronomy, University of Minnesota

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz2 Outline Novae and Galactic chemical evolution Outburst Development Physical properties of nova grains Gas Phase abundances Comparisons with ISM and the Solar System Grains Summary

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz3 A Classical Nova Explosion: Accretion followed by a TNR

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz4 The Role of Classical Novae in Galactic Chemical Evolution

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz5 Stardust and Stellar Evolution

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz6 IR/Radio Development Phases R. D. Gehrz (1988, 1990) The luminosity of the outburst fireball is L o  L Edd c measures n H and the ejected ionized gas mass M gas during the free-free expansion phase (10 -4 M  ) L o  L Edd = L IR for optically thick dust shells  L o = constant for a long time in  m Fireball Expansion Phase Free-Free Expansion Phase Coronal Phase in ONeMg Novae Dust Cocoon Phase in CO Novae

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz7 Physical Parameters Derivable from IR SED’s and Spectra T BB in K and time of the outburst t o in JD for expanding photospheres and dust shells The apparent luminosity; for blackbodies, f = 1.36 ( f ) max in W cm -2 The free-free self-absorption wavelength c in  m The outflow velocity V o in Km s -1 from emission lines

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz8 Mass of the Ejecta from IR SED’s From Thomson scattering, which dominates the shell opacity during the fireball/free-free transition: From c during the optically thin free-free phase: M gas  1-3x10 -4 M  for ONeMg WD’s M gas  1-5x10 -5 M  for CO WD’s in M  These methods are independent of D as long as V o is known from IR spectra

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz9 Dust Condensation in CO Novae R. D. Gehrz (1988, 1990) Dust Formation in NQ Vul Visual Transition  L o  L Edd = L IR T c = 1000K T c  1000 K, where V o is the outflow velocity

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz10 IR Spectra of Dust Grains: Molecular Structure Silicates: SiO 2 bond stretching and bending vibrational mode emission at 10  m and 20  m Silicon Carbide: SiC stretching vibrational mode emission at 11.3  m Carbon and iron: Smooth emissivity Hydrocarbons (HAC and PAH): C-H stretch at 3.3  m and other stretching modes at longer wavelengths

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz11 Nova Grain Properties Novae produce carbon, SiC, silicates, and hydrocarbons Abundances can be derived from visual opacity, IR opacity, and IR emission feature strength The grains grow to radii of  m

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz12 Amorphous Carbon Grains in the Ejecta of NQ Vul, LW Ser, and V1668 Cyg Gehrz et al. 1984, ApJ, 281, 303 Gehrz 1988, ARA&A, 26, 377 Iron seems not to be an option based on abundance arguments

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz13 Carbon and SiC Grains in Nova 1370 Aql (1982) Data from Gehrz et al. 1984, ApJ, 281, 303

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz14 Grain Condensation in V842 Cen (1986) From R. D. Gehrz, 1990, in Physics of Classical Novae, eds. A. Cassatella and R. Viotti, Springer-Verlag: Berlin, p Amorphous Carbon Hydrocarbons Silicates

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz15 Grain Condensation in Nova QV Vul 1987 (2) Carbon, Silicates, SiC, and PAH grains formed at different epochs suggesting abundance gradients in the ejecta. A. D. Scott (MNRAS, 313, (2000)) has shown that this could be explained by an asymmetric ejection due to a TNR on a rotating WD

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz16 Grain Condensation in V705 Cas (1993) s Free-free, amorphous carbon, silicates, and hydrocarbon UIR emission are required to fit the IR spectrum in detail. There are many variables – constraining data are needed

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz17 Modeling the IR SED of V705 Cas (1993) There are many variables – constraining data are needed See C. Mason et al. 1998, ApJ, 494, 783

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz18 Grain Mass, Abundance, and Size M dust from the infrared luminosity of the dust shell: Abundance of the grain condensables is given by: Grain radius from the optical depth of the visual transition and L IR : in M  compared to solar abundance in  m(a gr   m)

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz19 Hydrocarbon Dust in Two Recent Novae

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz20 Comets as the “Rosetta Stone” of the Solar System They are the remaining “planetesimals” from the epoch of planet formation in the primitive Solar nebula The material released from comet nuclei during perihelion passage is therefore a sample of the content of this primordial environment IR imaging photometry and spectroscopy can be used to deduce the composition and physical properties of the gas, dust, and ices present when the planets were forming

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz21 SOFIA and Comets: Mineral Grains What can SOFIA observations of comets tell us about the origin of the Solar System? Comet dust mineralogy: amorphous, crystalline, and organic constituents Comparisons with IDPs and meteorites Comparisons with Stardust Only SOFIA can make these observations near perihelion The vertical lines mark features of crystalline Mg-rich crystalline olivine (forsterite) ISO Data Spitzer Data

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz22 Comet Grain Properties

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz23 Comet Dust and Nova Dust Compared Comet Hale-Bopp Both Comet dust and nova dust contain silicates and carbon Comets have coma emission dominated by grains the size of those produced in nova outflows a gr  0.2  ma gr  0.7  m r = 1.21 AU  T BB = 253K

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz24 Novae and the Primitive Solar System: Interplanetary Dust Particles (IDPs) IDP’s are composed of sub micron grains within a “Cluster of Grapes” fractal structure tens to hundreds of microns across IDP sub- grains are similar in structure, size, and composition to nova “stardust” IDP’s have Carbon, Silicate, and hydrocarbon components seen in nova grains

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz25 On the Nature of the Dust in the Debris Disk around HD C. M. Lisse, C. A. Beichman, G. Bryden, and M. C. Wyatt The Astrophysical Journal, 658:584–592, 2007 March 20 Using a robust approach to determine the bulk average mineralogical composition of the dust, we show it to be substantially different from that found for comets 9P/Tempel 1 and C/ Hale-Bopp 1995 O1 or for the comet- dominated YSO HD Lacking in carbonaceous and ferrous materials but including small icy grains, the composition of the HD dust most closely resembles that of a disrupted P- or D-type asteroid.

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz26 Abundances from IR Forbidden Emission Lines Hayward et al. 1996, ApJ, 469, 854Gehrz et al. 1985, ApJ, 298, L47 Greenhouse et al. 1988, AJ, 95, 172

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz27 SOFIA and Classical Nova Explosions What can SOFIA tell us about gas phase abundances in Classical Nova Explosions? Gas phase abundances of CNOMgNeAl Contributions to ISM clouds and the primitive Solar System Kinematics of the Ejection

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz28 Abundance Anomalies in “Neon” Novae ONeMg TNR’s can produce and excavate isotopes of CNO, Ne, Na, Mg, Al, Si, Ca, Ar, and S, etc. that are expelled in their ejecta ONeMg TNR’s are predicted to have highly enhanced 22 Na and 26 Al abundances in their outflows. These isotopes are implicated in the production of the 22 Ne (Ne-E) and 26 Mg abundance anomalies in Solar System meteoritic inclusions : 22 Ne via: 22 Na  22 Ne + e + +  (  1/2 = 2.7 yr) 26 Mg via: 26 Al  26 Mg + e + +  (  1/2 = 7  10 5 yr)

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz29 Classical Novae and Abundance Anomalies Gehrz, Truran, and Williams 1993 (PPIII, p. 75) and Gehrz, Truran, Williams, and Starrfield 1997 (PASP, 110, 3) have concluded that novae may affect ISM abundances: Novae process  0.3% of the ISM (dM/dt) novae  7x10 -3 M  yr -1 (dM/dt) supernovae  6x10 -2 M  yr -1 Novae may be important on a global Galactic scale if they produce isotopic abundances that are  10 times SN and  100 times Solar; Ejected Masses calculated from IR/Radio methods give a lower limit

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz30 Chemical Abundances in Classical Novae from IR Data (1) NovaXY(n X / n Y ) nova (n X / n Y )  Reference LW SerCarbon dustH  15 Gehrz et al. 1980a QU VulAlSi 70Greenhouse et al V1974 CygNeSi  35 Gehrz et al V705 CasSilicatesH  17 Gehrz et al. 1995a V1974 CygNH  50 Hayward et al V1974 CygOH  25 Hayward et al V1974 CygNeH  50 Hayward et al. 1996

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz31 Chemical Abundances in Classical Novae from IR Data (2) NovaXY(n X / n Y ) nova (n X / n Y )  Reference V705 CasCarbon dustH  45 Mason et al V705 CasCaH 20Salama et al (ISO) V705 CasOH  25 Salama et al (ISO) V705 CasCarbon dustH  20 Mason et al V1425 AqlNHe  100 Lyke et al (ISO) CP CruNH 75Lyke et al (ISO) CP CruOH 17Lyke et al (ISO) CP CruNeH 27Lyke et al (ISO)

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz32 Chemical Abundances in Classical Novae from IR Data (3) NovaXY(n X / n Y ) nova (n X / n Y )  Reference QU VulNeH  168 Gehrz et al (Spitzer) QU VulOH  2.3 Gehrz et al (Spitzer)

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, Ne (10 -3 cm 3 STP g -1 IDP) - 22 Ne (10 -3 cm 3 STP g -1 IDP) - Anomalous IDPs Normal IDPs Normal GSC IDPs Anomalous GSC IDPs Normal TTC IDPs Anomalous TTC IDPs 20 Ne/ 22 Ne (Solar Wind) = 13.9

Ne (10 -3 cm 3 STP g -1 IDP) - 22 Ne (10 -3 cm 3 STP g -1 IDP) - Anomalous IDPs Normal IDPs Normal GSC IDPs Anomalous GSC IDPs Normal TTC IDPs Anomalous TTC IDPs 20 Ne/ 22 Ne (Solar Wind) = 13.9

Isotope Ratios 3 He/ 4 He 4 He/ 20 Ne 20 Ne/  22 Ne 20 Ne/ 21 Ne    <10 -8   21 Ne/  22 Ne Solar Wind Neon Nova  Neon Novae range SN II range

Isotope Ratios 3 He/ 4 He 4 He/ 20 Ne 20 Ne/  22 Ne 20 Ne/ 21 Ne    <10 -8   21 Ne/  22 Ne Solar Wind Neon Nova  Neon Novae range SN II range

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, Isotope Ratios 3 He nd 3 He/ 4 He 4 He/ 20 Ne 21 Ne/  22 Ne 20 Ne/  22 Ne 20 Ne/ 21 Ne    <10 -8   Anomalous IDPs Normal IDPs Neon Nova  Neon Novae range Solar Wind

Isotope Ratios 3 He nd 3 He/ 4 He 4 He/ 20 Ne 21 Ne/  22 Ne 20 Ne/  22 Ne 20 Ne/ 21 Ne    <10 -8   Anomalous IDPs Normal IDPs Neon Nova  Neon Novae range Solar Wind

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz39 Summary and Conclusions IR/Radio data yield quantitative estimates for physical parameters characterizing the nova outburst: D, L o, M gas, T dust, a dust, M dust, V o, L o, grain composition, and elemental abundances Nova ejecta produce all known types of astrophysical grains: amorphous carbon, SiC, hydrocarbons, and silicates Classical Nova ejecta have large overabundances (factors of 10 to 100) of CNO, Ne, Mg, Al, S, Si

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz40 Summary and Conclusions: Pre-Solar Clouds IR/Radio data show that the mineral composition and size distribution of the “stardust” made by novae are similar to those of the small grains released by comets in the Solar System IR/Radio data confirms theoretical predictions suggesting that nova TNRs can produce ejecta that lead to 22 Ne (Ne-E) and 26 Mg enhancements such as are seen in meteorites Novae are therefore a potential source for at least some of the solids that were present in the primitive Solar Nebula Novae are therefore a potential source for at least some of the solids that were present in the primitive Solar Nebula

Grains and Gas in Classical Nova Ejecta Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz41 Future Research Physical parameters and abundances must be obtained for a larger sample of novae to improve statistics Observations of stellar populations in M33 will be conducted using SIRTF to understand the global galactic contributions of classical novae Further examination of IDPs and meteoritic inclusions should be made to identify pre-solar grains from novae