Grains and Gas in Classical Nova Ejecta Grains

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Grains and Gas in Classical Nova Ejecta Grains and Gas in the Ejecta of

Grains and Gas in Classical Nova Ejecta Grains and Gas in the Ejecta of Classical Novae R. D. Gehrz Department of Astronomy, University of Minnesota 1 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Outline • Novae and Galactic chemical evolution

Grains and Gas in Classical Nova Ejecta 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 2 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta A Classical Nova Explosion: Accretion followed by

Grains and Gas in Classical Nova Ejecta A Classical Nova Explosion: Accretion followed by a TNR 3 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta The Role of Classical Novae in Galactic

Grains and Gas in Classical Nova Ejecta The Role of Classical Novae in Galactic Chemical Evolution 4 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Stardust and Stellar Evolution 5 Presolar Grains

Grains and Gas in Classical Nova Ejecta Stardust and Stellar Evolution 5 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta IR/Radio Development Phases • The luminosity of

Grains and Gas in Classical Nova Ejecta IR/Radio Development Phases • The luminosity of the outburst fireball is Lo LEdd Fireball Expansion Phase • c measures n. H and the ejected ionized gas mass Mgas during the free-free expansion phase (10 -4 M ) Free-Free Expansion Phase Coronal Phase in ONe. Mg Novae Dust Cocoon Phase in CO Novae 6 in m • Lo LEdd = LIR for optically thick dust shells Lo = constant for a long time R. D. Gehrz (1988, 1990) Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Physical Parameters Derivable from IR SED’s and

Grains and Gas in Classical Nova Ejecta Physical Parameters Derivable from IR SED’s and Spectra • TBB in K and time of the outburst to 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 Vo in Km s-1 from emission lines 7 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Mass of the Ejecta from IR SED’s

Grains and Gas in Classical Nova Ejecta Mass of the Ejecta from IR SED’s • From Thomson scattering, which dominates the shell opacity during the fireball/free-free transition: in M • From c during the optically thin free-free phase: in M • Mgas 1 -3 x 10 -4 M for ONe. Mg WD’s • Mgas 1 -5 x 10 -5 M for CO WD’s These methods are independent of D as long as Vo is known from IR spectra 8 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Dust Condensation in CO Novae Dust Formation

Grains and Gas in Classical Nova Ejecta Dust Condensation in CO Novae Dust Formation in NQ Vul Visual Transition • Tc 1000 K • Lo LEdd = LIR Tc = 1000 K • , where Vo is the outflow velocity R. D. Gehrz (1988, 1990) 9 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta IR Spectra of Dust Grains: Molecular Structure

Grains and Gas in Classical Nova Ejecta IR Spectra of Dust Grains: Molecular Structure • Silicates: Si. O 2 bond stretching and bending vibrational mode emission at 10 m and 20 m • Silicon Carbide: Si. C 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 10 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Nova Grain Properties • Novae produce carbon,

Grains and Gas in Classical Nova Ejecta Nova Grain Properties • Novae produce carbon, Si. C, silicates, and hydrocarbons • Abundances can be derived from visual opacity, IR opacity, and IR emission feature strength • The grains grow to radii of 0. 2 -0. 7 m 11 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Amorphous Carbon Grains in the Ejecta of

Grains and Gas in Classical Nova Ejecta Amorphous Carbon Grains in the Ejecta of NQ Vul, LW Ser, and V 1668 Cyg Gehrz 1988, ARA&A, 26, 377 Iron seems not to be an option based on abundance arguments 12 Gehrz et al. 1984, Ap. J, 281, 303 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Carbon and Si. C Grains in Nova

Grains and Gas in Classical Nova Ejecta Carbon and Si. C Grains in Nova 1370 Aql (1982) Data from Gehrz et al. 1984, Ap. J, 281, 303 13 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Grain Condensation in V 842 Cen (1986)

Grains and Gas in Classical Nova Ejecta Grain Condensation in V 842 Cen (1986) • Amorphous Carbon • Hydrocarbons • Silicates From R. D. Gehrz, 1990, in Physics of Classical Novae, eds. A. Cassatella and R. Viotti, Springer-Verlag: Berlin, p. 138. 14 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Grain Condensation in Nova QV Vul 1987

Grains and Gas in Classical Nova Ejecta Grain Condensation in Nova QV Vul 1987 (2) • Carbon, Silicates, Si. C, and PAH grains formed at different epochs suggesting abundance gradients in the ejecta. • A. D. Scott (MNRAS, 313, 775 -782 (2000)) has shown that this could be explained by an asymmetric ejection due to a TNR on a rotating WD 15 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Grain Condensation in V 705 Cas (1993)

Grains and Gas in Classical Nova Ejecta Grain Condensation in V 705 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 16 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Modeling the IR SED of V 705

Grains and Gas in Classical Nova Ejecta Modeling the IR SED of V 705 Cas (1993) There are many variables – constraining data are needed See C. Mason et al. 1998, Ap. J, 494, 783 17 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Grain Mass, Abundance, and Size • Mdust

Grains and Gas in Classical Nova Ejecta Grain Mass, Abundance, and Size • Mdust from the infrared luminosity of the dust shell: in M • Abundance of the grain condensables is given by: compared to solar abundance • Grain radius from the optical depth of the visual transition and LIR: in m 18 (agr 0. 2 -0. 7 m) Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Hydrocarbon Dust in Two Recent Novae 19

Grains and Gas in Classical Nova Ejecta Hydrocarbon Dust in Two Recent Novae 19 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Comets as the “Rosetta Stone” of the

Grains and Gas in Classical Nova Ejecta 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 20 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta SOFIA and Comets: Mineral Grains What can

Grains and Gas in Classical Nova Ejecta SOFIA and Comets: Mineral Grains What can SOFIA observations of comets tell us about the origin of the Solar System? ISO Data Spitzer Data • Comet dust mineralogy: amorphous, crystalline, and organic constituents • Comparisons with IDPs and meteorites • Comparisons with Stardust The vertical lines mark features of crystalline Mg-rich crystalline olivine (forsterite) 21 • Only SOFIA can make these observations near perihelion Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Comet Grain Properties 22 Presolar Grains Workshop,

Grains and Gas in Classical Nova Ejecta Comet Grain Properties 22 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Comet Dust and Nova Dust Compared agr

Grains and Gas in Classical Nova Ejecta Comet Dust and Nova Dust Compared agr 0. 7 m agr 0. 2 m Comet Hale-Bopp r = 1. 21 AU TBB = 253 K • 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 23 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Novae and the Primitive Solar System: Interplanetary

Grains and Gas in Classical Nova Ejecta 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 24 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta On the Nature of the Dust in

Grains and Gas in Classical Nova Ejecta On the Nature of the Dust in the Debris Disk around HD 69830 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 9 P/Tempel 1 and C/ Hale-Bopp 1995 O 1 or for the cometdominated YSO HD 100546. Lacking in carbonaceous and ferrous materials but including small icy grains, the composition of the HD 69830 dust most closely resembles that of a disrupted P- or D-type asteroid. 25 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Abundances from IR Forbidden Emission Lines Greenhouse

Grains and Gas in Classical Nova Ejecta Abundances from IR Forbidden Emission Lines Greenhouse et al. 1988, AJ, 95, 172 Gehrz et al. 1985, Ap. J, 298, L 47 26 Hayward et al. 1996, Ap. J, 469, 854 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta SOFIA and Classical Nova Explosions What can

Grains and Gas in Classical Nova Ejecta SOFIA and Classical Nova Explosions What can SOFIA tell us about gas phase abundances in Classical Nova Explosions? • Gas phase abundances of CNOMg. Ne. Al • Contributions to ISM clouds and the primitive Solar System • Kinematics of the Ejection 27 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Abundance Anomalies in “Neon” Novae • ONe.

Grains and Gas in Classical Nova Ejecta Abundance Anomalies in “Neon” Novae • ONe. Mg 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 • ONe. Mg 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: 26 Mg 28 via: 22 Na 22 Ne +e+ + ( 1/2 = 2. 7 yr) 26 Al 26 Mg +e+ + ( 1/2 = 7 105 yr) Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Classical Novae and Abundance Anomalies Gehrz, Truran,

Grains and Gas in Classical Nova Ejecta 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 • (d. M/dt)novae 7 x 10 -3 M yr-1 • (d. M/dt)supernovae 6 x 10 -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 29 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Chemical Abundances in Classical Novae from IR

Grains and Gas in Classical Nova Ejecta Chemical Abundances in Classical Novae from IR Data (1) 30 Nova X Y (n. X/ n. Y)nova (n. X/ n. Y) LW Ser Carbon dust H 15 QU Vul Al Si 70 V 1974 Cyg Ne Si 35 V 705 Cas Silicates H V 1974 Cyg N H 50 Hayward et al. 1996 V 1974 Cyg O H 25 Hayward et al. 1996 V 1974 Cyg Ne H 50 Hayward et al. 1996 17 Reference Gehrz et al. 1980 a Greenhouse et al. 1988 Gehrz et al. 1994 Gehrz et al. 1995 a Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Chemical Abundances in Classical Novae from IR

Grains and Gas in Classical Nova Ejecta Chemical Abundances in Classical Novae from IR Data (2) 31 Nova X Y (n. X/ n. Y)nova (n. X/ n. Y) Reference V 705 Cas Carbon dust H 45 V 705 Cas Ca H 20 Salama et al. 1997 (ISO) V 705 Cas O H 25 Salama et al. 1997 (ISO) V 705 Cas Carbon dust H 20 Mason et al. 1998 V 1425 Aql N He 100 Lyke et al. 2002 (ISO) CP Cru N H 75 Lyke et al. 2003 (ISO) CP Cru O H 17 Lyke et al. 2003 (ISO) CP Cru Ne H 27 Lyke et al. 2003 (ISO) Mason et al. 1997 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Chemical Abundances in Classical Novae from IR

Grains and Gas in Classical Nova Ejecta Chemical Abundances in Classical Novae from IR Data (3) 32 Nova X Y (n. X/ n. Y)nova (n. X/ n. Y) Reference QU Vul Ne H 168 Gehrz et al. 2008 (Spitzer) QU Vul O H 2. 3 Gehrz et al. 2008 (Spitzer) Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

- Grains and Gas in Classical Nova Ejecta 0. 60 22 Ne (10 -3

- Grains and Gas in Classical Nova Ejecta 0. 60 22 Ne (10 -3 cm 3 STP g-1 IDP) Normal GSC IDPs Anomalous GSC IDPs 0. 50 Normal IDPs Normal TTC IDPs 20 Ne/22 Ne (Solar Wind) = 13. 9 0. 40 Anomalous TTC IDPs 0. 30 0. 20 0. 10 Anomalous IDPs 0. 00 0 1 2 3 4 5 20 Ne 6 7 8 9 10 (10 -3 cm 3 STP g-1 IDP) - Presolar Grains Workshop, St. Louis, MO, January 28, 2012 11 12 13 14

- 0. 60 22 Ne (10 -3 cm 3 STP g-1 IDP) Normal GSC

- 0. 60 22 Ne (10 -3 cm 3 STP g-1 IDP) Normal GSC IDPs Anomalous GSC IDPs 0. 50 Normal IDPs Normal TTC IDPs 20 Ne/22 Ne (Solar Wind) = 13. 9 0. 40 Anomalous TTC IDPs 0. 30 0. 20 0. 10 Anomalous IDPs 0. 00 0 1 2 3 4 5 20 Ne 6 7 8 9 (10 -3 cm 3 STP g-1 IDP) - 10 11 12 13 14

104 103 � 20 Ne/ 22 Ne 102 20 Ne/21 Ne � Isotope Ratios

104 103 � 20 Ne/ 22 Ne 102 20 Ne/21 Ne � Isotope Ratios 101 � 4 He/20 Ne 100 10 -1 � 10 -2 21 Ne/ 22 Ne 10 -3 3 He/4 He � Neon Nova 10 -4 10 -5 � <10 -8 Neon Novae range SN II range Solar Wind

104 103 � 20 Ne/ 22 Ne 102 20 Ne/21 Ne � Isotope Ratios

104 103 � 20 Ne/ 22 Ne 102 20 Ne/21 Ne � Isotope Ratios 101 � 100 4 He/20 Ne 10 -1 � 10 -2 21 Ne/ 22 Ne 10 -3 3 He/4 He � Neon Nova 10 -4 10 -5 � <10 -8 Neon Novae range SN II range Solar Wind

Grains and Gas in Classical Nova Ejecta 104 � 103 102 20 Ne/21 Ne

Grains and Gas in Classical Nova Ejecta 104 � 103 102 20 Ne/21 Ne � Isotope Ratios 101 � 20 Ne/ 22 Ne 100 21 Ne/ 22 Ne 4 He/20 Ne 10 -1 � 10 -2 10 -3 3 He/4 He Anomalous IDPs � Neon Nova 10 -4 10 -5 � <10 -8 3 He nd Neon Novae range Solar Wind Normal IDPs Presolar Grains Workshop, St. Louis, MO, January 28, 2012

104 � 103 102 20 Ne/21 Ne � Isotope Ratios 101 � 20 Ne/

104 � 103 102 20 Ne/21 Ne � Isotope Ratios 101 � 20 Ne/ 22 Ne 100 21 Ne/ 22 Ne 4 He/20 Ne 10 -1 � 10 -2 10 -3 3 He/4 He Anomalous IDPs � Neon Nova 10 -4 10 -5 � <10 -8 3 He nd Neon Novae range Solar Wind Normal IDPs

Grains and Gas in Classical Nova Ejecta Summary and Conclusions • IR/Radio data yield

Grains and Gas in Classical Nova Ejecta Summary and Conclusions • IR/Radio data yield quantitative estimates for physical parameters characterizing the nova outburst: D , Lo , Mgas , Tdust , adust , Mdust , Vo , Lo , grain composition, and elemental abundances • Nova ejecta produce all known types of astrophysical grains: amorphous carbon, Si. C, hydrocarbons, and silicates • Classical Nova ejecta have large overabundances (factors of 10 to 100) of CNO, Ne, Mg, Al, S, Si 39 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Summary and Conclusions: Pre-Solar Clouds • IR/Radio

Grains and Gas in Classical Nova Ejecta 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 40 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz

Grains and Gas in Classical Nova Ejecta Future Research • Physical parameters and abundances

Grains and Gas in Classical Nova Ejecta Future Research • Physical parameters and abundances must be obtained for a larger sample of novae to improve statistics • Observations of stellar populations in M 33 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 41 Presolar Grains Workshop, St. Louis, MO, January 28, 2012 R. D. Gehrz