Nucleosynthesis in classical nova explosions and Type I X-ray bursts

Transcription

1 Important and significant: lies the experimentalist told me Nucleosynthesis in classical nova explosions and Type I X-ray bursts Anuj Parikh Universitat Politècnica de Catalunya Institut d'estudis Espacials de Catalunya Barcelona, Spain Anuj Parikh Grup d Astronomia i Astrofísica Universitat Politècnica de Catalunya Institut d'estudis Espacials de Catalunya

2 Important and significant: lies the experimentalist told me Nucleosynthesis in classical nova explosions and Type I X-ray bursts Anuj Parikh Universitat Politècnica de Catalunya Institut d'estudis Espacials de Catalunya Barcelona, Spain

3 Important and significant: lies the experimentalist told me Nucleosynthesis in classical nova explosions and Type I X-ray bursts Anuj Parikh Universitat Politècnica de Catalunya Institut d'estudis Espacials de Catalunya Barcelona, Spain

4 Important and significant: lies the experimentalist told me Nucleosynthesis in classical nova explosions and Type I X-ray bursts Anuj Parikh Universitat Politècnica de Catalunya Institut d'estudis Espacials de Catalunya Barcelona, Spain

5 NUCLEAR ASTROPHYSICS Understand HOW the chemical elements were (and still are!) created Elemental composition of the Solar System Reviews: B2FH 1957, Cameron 1957, Rolfs and Rodney 1988, Iliadis 2007, José and Iliadis 2011

6 Understand the NUCLEOSYNTHESIS and ENERGY generation in different astrophysical phenomena CLASSICAL NOVA EXPLOSIONS: Explosive thermonuclear burning of accreted matter on the surface of a white dwarf star AU Nova Cygni 1992 (d ~ ly) Vanlandingham et al. (1997) Nova V693 CrA 1981 HST (1994) Reviews: Gehrz+ 1998, José and Hernanz 2007; Bode and Evans 2012

7 Understand the NUCLEOSYNTHESIS and ENERGY generation in different astrophysical phenomena TYPE I X-RAY BURSTS: Explosive thermonuclear burning of accreted matter on the surface of a neutron star Galloway et al. (2008) / RXTE 1 arcmin Reviews: Lewin+ 1993, Strohmayer and Bildsten 2006, AP, José, Sala and Iliadis 2013

8 Understand the NUCLEOSYNTHESIS and ENERGY generation in different astrophysical phenomena TYPE Ia SUPERNOVA EXPLOSIONS: White dwarf accretes matter until M Ch, white dwarf mergers,... SN1604 (Kepler) d = 5' SN2014J Chandra + Spitzer + HST X-ray + infrared + visible Ashell et al. (2014) Reviews: Livio 2000; Hillebrandt & Niemeyer 2000; Isern+ 2011; Howell 2011; Hillebrandt+ 2013

9 What nuclear reactions are involved in these phenomena? Classicalnova nucleosynthesis 150 isotopes (H Ca) 1000 nuclear processes José Z N MODELS: Schatzmann 1950, 1951; Starrfield 1971; Hillebrandt and Thielemann 1982; Wiescher et al. 1986; Weiss and Truran 1990; Prialnik and Kovetz 1995; Starrfield et al. 1998; Jose and Hernanz 1998; Paxton et al. 2011, Denissenkov et al. 2013,

10 What nuclear reactions are involved in these phenomena? Z TypeI X-rayburst nucleosynthesis 600 isotopes (H Xe) 4000 nuclear processes Schatz et al., nova N MODELS: Woosley and Taam 1976; Maraschi and Cavaliere 1977; Fujimoto et al 1981; Wallace and Woosley 1981; Hanawa et al. 1983; Schatz et al. 1999, 2001; Iliadis et al. 2002; Koike et al. 1999, 2004; AP et al. 2008; Wallace et al. 1982; Woosley and Weaver 1985; Taam et al. 1993; 1996; Woosley et al. 2004; Fisker et al. 2008; José et al. 2010; Paxton et al

11 What nuclear reactions are involved in these phenomena? Classicalnova nucleosynthesis 150 isotopes (H Ca) 1000 nuclear processes TypeI X-rayburst nucleosynthesis 600 isotopes (H Xe) 4000 nuclear processes TypeIasupernova nucleosynthesis 400 isotopes (H Zn) 2000 nuclear processes

12 What nuclear reactions are involved in these phenomena? Classicalnova nucleosynthesis 150 isotopes (H Ca) 1000 nuclear processes TypeI X-rayburst nucleosynthesis 600 isotopes (H Xe) 4000 nuclear processes TypeIasupernova nucleosynthesis 400 isotopes (H Zn) 2000 nuclear processes Are they all "important and significant"?

13 What nuclear reactions are involved in these phenomena? Classicalnova nucleosynthesis 150 isotopes (H Ca) 1000 nuclear processes TypeI X-rayburst nucleosynthesis 600 isotopes (H Xe) 4000 nuclear processes TypeIasupernova nucleosynthesis 400 isotopes (H Zn) 2000 nuclear processes Are they all "important and significant"? EQUALLY Just because a reaction CAN be measured does not mean it needs to be measured (for nuclear astrophysics)

14 What nuclear reactions are involved in these phenomena? Classicalnova nucleosynthesis 150 isotopes (H Ca) 1000 nuclear processes TypeI X-rayburst nucleosynthesis 600 isotopes (H Xe) 4000 nuclear processes TypeIasupernova nucleosynthesis 400 isotopes (H Zn) 2000 nuclear processes Are they all "important and significant"? EQUALLY Just because a reaction CAN be measured does not mean it needs to be measured (for nuclear astrophysics) Sensitivity study: Vary nuclear reaction rates in a model by uncertainties Identify those rates that significantly affect model predictions of observables from astrophysical phenomena Improve these rates first!

15 How robust is nucleosynthesis in classical novae to variations in the nuclear physics input? Reaction rates with demonstrated impact on nova nucleosynthesis in at least two independent studies << 1000 reactions! Review: AP, José, Sala (2014)

16 How robust is nucleosynthesis in classical novae to variations in the nuclear physics input? Reaction rates with demonstrated impact on nova nucleosynthesis in at least two independent studies << 1000 reactions! Review: AP, José, Sala (2014)

17 How robust is nucleosynthesis in classical novae to variations in the nuclear physics input? MOST nuclear reaction rates involved in standard models now "seem to be" sufficiently well-constrained. Effect of an updated reaction network on nucleosynthesis predictions With data from Starrfield+ (2009) José and Iliadis (2011)

18 18 F(p,α) 15 O in CN Experiments: Chae+ 2006, de Sereville+ 2009, Murphy+ 2009, Beer+ 2011, Dalouzy+ 2009, Adekola+ 2011a, 2011b, 2012, Laird Laird, AP++ (2013) experimental rate varied within uncertainties 1D hydro nova model γ-ray emission from novae may initially be dominated by contributions from e+-e- following 18 F(β+) (t 1/2 = 110 m)

19 30 P(p,γ) 31 S in CN Experiments: Jenkins+ 2006, Ma+ 2007, Wrede+ 2007, 2009, AP+ 2011, Doherty+ 2012, Irvine AP++ (2011) experimental rate varied within uncertainties 1D hydro nova model

20 33 S(p,γ) 34 Cl in CN Experiments: Waanders+ 1983, AP+ 2009, Freeman+2011, Fallis+ 2013, AP AP++ (2014) experimental rate varied within uncertainties 1D hydro nova model

21 How robust is nucleosynthesis in type I XRBs to variations in the nuclear physics input? MOST nuclear reaction rates involved in XRBs are NOT based on experimental information. need to rely on estimates from nuclear theory... theoryvs experiment factor of 2 theory1 vs theory2 AP, José, Sala and Iliadis(2013)

22 How robust is nucleosynthesis in type I XRBs to variations in the nuclear physics input? ReactionrateswithdemonstratedimpactonXRB propertiesin at least two independent studies << 4000 reactions! + 57 Cu(p,γ), 59 Cu(p,γ), 61 Ga(p,γ), 65 As(p,γ) + masses: 62 Ge, 66 Se... Review: AP, José, Sala (2014)

23 How robust is nucleosynthesis in type I XRBs to variations in the nuclear physics input? ReactionrateswithdemonstratedimpactonXRB propertiesin at least two independent studies << 4000 reactions! + 57 Cu(p,γ), 59 Cu(p,γ), 61 Ga(p,γ), 65 As(p,γ) + masses: 62 Ge, 66 Se... Review: AP, José, Sala (2014)

24 14 O(α,p) 17 F in XRBs Experiments: Hahn+1996, Park+1999, Harss+ 1999, 2002, Blackmon+ 2001, 2003, Gomez del Campo+ 2001, Notani+ 2004, He+ 2009, 2011, Bardayan+ 2010, 2012, Almaraz-Calderon Blackmon XRB postprocessing model Hu, He, AP++ (2014)

25 18 Ne(α,p) 21 Na in XRBs Experiments: Chen+2001, Caggiano+2002, Berg+2003, Matic+2009, Chae+2009, He+2008, 2009, Bradfield-Smith+1999, Groombridge+2002, Salter XRB postprocessing model Matic et al D hydro model He, Zhang, AP++ (2013)

26 18 Ne(α,p) 21 Na in XRBs Experiments: Chen+2001, Caggiano+2002, Berg+2003, Matic+2009, Chae+2009, He+2008, 2009, Bradfield-Smith+1999, Groombridge+2002, Salter XRB model discrepancies? XRB postprocessing model lower rate higher rate Matic et al D hydro model He, Zhang, AP++ (2013)

27 15 O(α,γ) 19 Ne in XRBs Experiments: Magnus+1990, Laird+2002, Davids+2003ab, Rehm+2003, Visser+2004, Tan+2005, 2007, 2009, Kanungo+2006, Mythili+2008 Fisker et al. 2007, 1D hydro model Davids et al. 2011, 1D hydro model lower rate higher rate XRB model discrepancies?

28 Weak interaction rates in XRBs? AP+ 2008

29 Decay rate (s -1 ) Nacher+, CERN proposal Weak interaction rates in XRBs? Sarriguren 2011 AP+ 2008

30 Type Ia supernova explosions Chandra + XMM, X-ray Chandra, VLA, CTIO X-ray + radio + visible Chandra + Spitzer X-ray + infrared Chandra + Spitzer + HST X-ray + infrared + visible SN185 (1st SN recorded) D 9000 ly d = 45' SN1006 D 7000 ly d = 55' SN1572 (Tycho) D 9000 ly d = 11' SN1604 (Kepler) D ly d = 5' Responsible for 50% of Fe-group element production in the Galaxy

31 Type Ia supernova explosions MODELS The increasing number of supernovae discovered has revealed some diversity among SNe Ia, raising doubts upon the uniqueness of the progenitor system [Branch+93, Li+11...] Promising progenitor scenarios include... Single degenerate: CO WD accretes H/He-rich matter until M Ch [Whelan+Iben73] Double degenerate: two merging CO WDs, M tot > M Ch [Iben+Tutukov84, Webbink84] R. Pakmor+ (MPA)

32 Type Ia supernova explosions MODELS The increasing number of supernovae discovered has revealed some diversity among SNe Ia, raising doubts upon the uniqueness of the progenitor system [Branch+93, Li+11...] Promising progenitor scenarios include... Single degenerate: CO WD accretes H/He-rich matter until M Ch [Whelan+Iben73] Double degenerate: two merging CO WDs, M tot > M Ch [Iben+Tutukov84, Webbink84] Detailed predictions of nucleosynthesis exist only for a very limited set of single degenerate scenario models Thielemann+ 1986; Nomoto+ 1997; Woosley 1997; Iwamoto+ 1999;Travaglio+ 2004; Röpke García-Senz+ 2007; Meakin+ 2009; Maeda+ 2010; Seitenzahl R. Pakmor+ (MPA)

33 How robust is nucleosynthesis in Type Ia SNe to variations in the nuclear physics input? Two M Ch explosion models (single degenerate) several million individual calculations Novae (Iliadis+02) 7000 calc XRBs (AP+08) calc standard yields Search for common processes that significantly affect nucleosynthesis AP, José, Seitenzahl, Röpke (2013)

34 How robust is nucleosynthesis in Type Ia SNe to variations in the nuclear physics input? << 2000 reactions! yields of Fe group species (Z > 23) are relatively robust to rate changes for these models Bravo, Martínez-Pinedo 2012; AP, José, Seitenzahl, Röpke 2013

35 Just because a reaction CAN be measured does not mean it needs to be measured (for nuclear astrophysics) SOME FUTURE WORK: modelers: extended multid model calculations of novae and XRBs + with larger nuclear reaction networks modelers: nuclear physics sensitivity studies using 1D hydrodynamic models for novae and XRBs + different models for SNIa modelers: evaluate the importance of the 14 O(α,p), 15 O(α,γ), 18 Ne(α,p) rates in XRBs modelers: evaluate if mass may be ejected in XRB models through radiation-driven winds experimentalists: measure/confirm "important and significant" reaction rates (+ nuclear masses) observers: prospects for more spectra from XRBs? (+improved models of NS atmospheres) development of improved, consistent treatments for calculating stellar weak interaction rates for all isotopes in typical SNIa and XRB networks