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http://pos.sissa.it AGB stars, as inferred inferred as stars, AGB xplosions. Laboratory studies of of studies Laboratory xplosions. r- to micrometer-sized presolar grains that grains that presolar r- to micrometer-sized identified presolar are silicon carbide These grainsThese incorporated from the matter outer and on the types of stars that on the types of ISM, and physical processes in the ars or in the ejecta of stellar e ejecta of stellar or in the ars eative Commons Attribution-NonCommercial-ShareAlike Licence. Licence. Commons Attribution-NonCommercial-ShareAlike eative

1 [email protected] [email protected] Speaker Speaker H-rich zone down to the innermost Ni-rich zone in variable proportions, as indicated by specific specific by indicated as proportions, variable zone in Ni-rich innermost the to down zone H-rich grains, SN of understanding our advanced have findings recent of couple A fingerprints. isotopic providinginsights ,new into SN dust chemistry, and formation. individual presolar grains have provided a wealth of astrophysical information, such as on stellar on stellar as such information, of astrophysical wealth a provided have grains presolar individual in formation grain evolution, chemical Galactic stars, in mixing and evolution, nucleosynthesis and stellar environments, chemical contributed dust to Among theSystem. the Solar ,(SiC), , refractoryoxides , and silicates. The isotopic ratios of the major of indicative magnitude, of orders many over range grains presolar in elements minor and (ca. 90 oxide/silicate (>90 %) and SiC presolar Most sources. stellar different from contributions intermediate-massw- to of lo winds the in formed apparently grains %) mainly heavy isotopic from element compositions (SiC) and, respectively, O-isotopic ratios II Type from grains stars, AGB from grains than abundant less Although (oxides/silicates). importance. of particular are (SNe) supernovae Primitive materials contain nanomete contain materials system solar Primitive in the winds of evolved st formed 1 Copyright ownedCopyright by the author(s) under the terms of the Cr

XI - NIC Cosmos the in Nuclei on Symposium 11th Germany Heidelberg, July 19–232010

Peter Hoppe Max Planck Institute for Chemistry Germany 55128 Mainz, 27, J.-J. Becherweg E-mail: of presolar grains Measurements

PoS(NIC XI)021 , 3 O 2 contained interstellar contained interstellar ary formed system by are from AGB stars. Photo AGB stars. from are AGB) star or a SN, and the AGB) star or a SN, and the buted dust to the solar system.buted dust to , lower left), and a grain consisting consisting and a grain left), , lower 4 O 2 Pictures of presolar grains from primitive primitive from grains presolar of Pictures SiC other presolar minerals have been SiC other presolar minerals carbide (SiC), were physically carbide (SiC), and 6 Gy of the ago, most ion (SIMS), resonance and co-workers at the University of Chicago leosynthesismixing in stars, and evolution, ), in which pristine interstellar grains can be ), in which pristine studies of single grains; the C-isotopic C-isotopic isotope studies of single grains; the ation in stellar environments, chemical and chemical ation in stellar environments, llar origin is still not clear. This is because llar origin ll fraction of it survived unaltered inside small ll fraction of it survived terstellar medium (ISM). Dust forms terstellar around medium millions of diamonds, is essentially solar and millions presolar SiC represents a sample of . of an Al-rich core surrounded by a silicate mantle mantle a silicate by core surrounded Al-rich of an (lowerright). TheSiC grain shown is from a an from grain graphite the (SN), ( branch giant asymptotic and silicate grains Institutecredit:Planck Max for Chemistry. Figure 1. Figure right), (upper graphite left), (upper SiC : spinel (MgAl

of our knowledge on presolar grains (section 2), of our knowledge on presolar grains (section 2), 2 ejecta of stellar explosions (Table 1) [3-5]. ejecta of stellar explosions (Table 1) [3-5]. Fragments from these bodies reach the Earth as Fragments these from m (Fig. 1). This permits m (Fig. 1). grain isotope studies and single This permits  on the types stars that contri of m hite p m  0.2  1 Silicate Gra ), and a variety of silicates. Like SiC, all these presolar haveminerals 19 O 12 Peter Hoppe Peter , and CaAl 4 O m 2 Laboratory especially studies, by secondary Following the discovery of presolar diamond and discovery presolar diamond Following the of Dust is an important the in constituent of Dust is an important silicon and grains, diamond The first presolar m  2 0.5  SiC Spinel physical processes in the ISM, and Here, I will briefly review the current state ionization mass spectrometry(RIMS), and electron microscopy, have provided a wealth of astrophysical information, such as on stellar nuc Galactic chemical evolution (GCE), grain form it was shown that all these presolar minerals are not only grains have but must interstellar formed in the winds of evolved stars or in the 1. Introduction 1. Introduction Presolar Grains Presolar MgAl found in the last two decades, namely, graphite, silicon nitride, refractory oxides (mainly Al refractoryoxides silicon nitride, graphite, two decades, namely, found in the last Whether also most of the diamonds have a ste diamonds of the Whether also most sizes >100 nm and sometimes even >1 in the 1980s [1-2]. It became quicklyin the 1980s [1-2]. clear that in size, which prevents 2-3 nm are only diamonds of grains, containing of ensembles composition isotope anomalies elements (e.g., Xe and Te) which,minor pronounced are seen only for however, maycarried only be by a small fraction of the grains. meteorites and interplanetary dust particles (IDPs isolated from chemically Ed Anders meteorites by our and its planet our Sun possibly also in the ISM. When evolved stars and 4. of gravitational collapse an interstellar cloud some dust was destroyed Onlyheavily altered. or a sma planetary bodies, the and . Because thesecompositions. isotopic our grains are anomalous identified by their than older “presolarsolar system they grains”. have been named PoS(NIC XI)021 2% 1% 5% 70% 70% 15% 10% <5% <1% 0.3% 0.3% 0.1% 100% 100% ~60% ~60% ~30% <10% >90% C and Contr. 13 Al (half 26 C/ AGBstars 12  Tc (half life 99 ) )   , CBP)  . The intermediate- . The -3 rs, post-AGB post-AGB rs, SN grains (section 3), (section SN grains SNII SNII SNII SNII AGB Novae Novae Novae (<1.8 M (<1.8 (low M & Z), SNII SNII & Z), M (low and 10 AGB (1.5-3 M AGB (1-2.2 M -4 AGB AGB J-type C sta J-type C stars, post-AGB post-AGB J-type C stars, high (H) temperatures, respectively; respectively; (H) temperatures, high V 49 2 O O Tc in SiC MS grains [9]. Silicon in MS in MS Silicon MS grains [9]. Tc in SiC O V Si 16 itions, presolar SiC can be divided into 18 99 Ti, 18 49 N 30 Ti d Si-isotopic systematics of the MS grains Although Si is affected by the s-process Although Si is in O/ SNII SNII Al 44 Mg from the decayMg from of radioactive 15 44 18 26 26 Ti, e first direct observational evidence that the e first direct observational evidence that the Si 44 are the mainstream (MS) grains which make up (MS) grains which make are the mainstream

O Ca, ced our understanding of ced our understanding Na (half-life 2.6 yr). (half-life Na 30 16 41 3 22 Si; Ne-E(L) Al, Al, have predominantly lower than solar Si, 30 C 26 Al, ; s-process elem. elem. ; s-process 29 13 2 ces The detection of radioactive [7]. O; extinct 26 N; enhanced enhanced N; Si; extinct 18 C/ C, 15 28 12 12 ubgrain composition composition ubgrain N/ Si plot, Fig. 3) must thus represent a range of starting 3) must plot, Fig. Si N, 14 O or O or 30 15 Si; ext. C, often enhanced enhanced often C, 16 O, strongly depleted depleted O, strongly Low Si; extinct O, depleted or ~ solar solar ~ or depleted O, 28 13 C, 17 O, lower than solar 28 C; enhanced enhanced C; 17 N; Ne-E(H) 13 Al ratios are typicallyAl ratios between 10 16 C/ 13 Ru from the decayRu from of O, Isotopic Signatures Isotopic Signatures Stellar Source Rel. 14 Slightly enhanced 27 Ne that is released at low (L) and at low released Ne that is N, 12 C/ 18 Enhanced Enhanced 99 O/ C/ 22 15 12 C, 17 12 Al/ Si vs.  N, 13 26 29 15 Low Enhanced Enhanced the decay of short-lived the decay of short-lived N. They carry radiogenic N. Enh. Low Enhanced Enhanced Presolar minerals with stellar origins from primitive meteorites. primitive meteorites. with stellar origins from Presolar minerals Enhanced Enhanced Low s-process elem.; s High 15 Enh. Enh. Enh. Enh. N/ 14

1 3 Peter Hoppe Peter Table 1.

50/ 50/ 200 Enhanced Enhanced 0.002 (ppm)

Based on the C-, N-, and Si-isotopic compos The most importantThe and the stellar isotopic signatures most sources of presolar minerals are 4 N 3 Reported maximum values (normalized to volume of matrix). matrix). of meteorite volume to (normalized values maximum Reported Higher abundances are observed isotopically primitive in IDPs. ) Ne-E: Almost monoisotopic monoisotopic Almost ) Ne-E: and present some unsolved problems (section 4). problems some unsolved and present distinct populations (Fig. 2) [6]. Most abundant [6]. (Fig. 2) distinct populations about 90% of all SiC grains. These grains of about solar as stellar sour metallicity 200000 y) in the spectra of giant stars was th giant stars the spectra of y) in 200000 chemical elements are Particularly produced in the interior of stars interesting in this respect[8]. radiogenic of is the finding mass and heavy exhibit elements the signature of the s-process, pointing to 1.5-3 M higher than solar higher than compositions of the parent stars established by the GCE of the Si [10-12]. [10-12]. of the Si isotopes stars established by the GCE of the parent compositions life 700000 y); inferred life 700000 1) 2 3) sources 2. Isotopic compositions and stellar Si Oxides/ silicates Graphite 10 Graphite Abund. Abund. 30 SiC Presolar Grains Presolar discuss several advan that have recent findings Ne-E(L) is probably from from is probably Ne-E(L) (slope 1.37 line in a  line (slope 1.37 solar Si is expected to change the envelope Si- metallicity AGB stars, the dredge-up of s-process The observe marginally. isotopic composition only grains shows only small isotope anomalies (<20%). grains shows only small isotope anomalies summarized in I will focus Table 1. In the follwing on three types of presolar grains, namely, silicates. SiC, oxides, and 2.1 PoS(NIC XI)021

C 13 C/ 12 Ti from the Ti from the N ratios (Fig. N ratios 49 15 N/ 14 Ca and 44 C and Carbon- and N-isotopic N-isotopic and Carbon- 13 Si ratios (Fig. 3). They have C/ 28 12

. C ratios of <10, a large range of <10, a C ratios of Si/ 13 30 C/ [3-5]

2. Figure presolar of different the compositions SiC populations. The solar ratios are Data lines. the dashed by indicated sources: [16-19] for the unusual and see grains other for the grains; C Type 12 Si and 28 of SiC grains from SNeII with isotopically SNeII with isotopically of SiC grains from ns are the presolar silicon nitride grains, all of ns are the presolar silicon nitride grains, all of Si/ resolution isotope mapping of thin sections of thin of mapping isotope resolution m low-m and intermediate mass stars AGB with V (half life 330 d). These isotopic signatures signatures V (half life 330 d). These isotopic 29 Mo) that can be explained by a neutron burst in a neutron burst explained by that can be Mo)

49 e refractory presolar oxides, cannot be separatede refractory 97 4 S made their discovery possible [28]. [28]. S made their discoverypossible Mo and

95 solar Al ratios somewhat higher than in MS grains make grains up the A and B higher than in MS Al ratios somewhat make if diamonds (Table 1). The reason for this is that they,are ignored if diamonds 27 Si (Fig. 3) [26]. It should be noted that not all grains with low noted that not be It should (Fig. 3) [26]. Si N, and lower than solar and N, Al/ 30 Ti (half life 60 y) and y) and life 60 Ti (half 15 26 44 Al ratios of up to nearly 1 and they carry radiogenic Al ratios of up to nearly carry1 and they radiogenic 27 Peter Hoppe Peter Al/ 26 rare are SiC grains from novae which have very low N are from novae since also SN grains with this signature have been found [27]. [27]. have been found novae since also SN grains with this signature N are from 15

N/ SiC grains from SNe are the These X grains grains are[20-23]. characterized by enhanced Very e Y and Z grains plot to the right of the SiC MS line, the signature of s-process Siline, the signature of the SiC MS the right Z grains plot to The Y and An important finding in the last decadeAn important was the discovery of presolar silicates. These

14 N N/

15 14 grains) and C (most which apparently come from SNe A new typewhich apparently come [25]. heavy Si was recently discovered and will be discussed in section 3. shocked He-rich matter Related[24]. to the X grai N-isotopic ratios, and N-isotopic ratios, 2.2 Oxides and silicates the most are they out, turned although, as it finally time for a long unrecognised grains remained mineral abundant presolar grains and th presolar contrary to carbonaceous chemically from meteorites and only high spatial high meteorites and only from chemically meteorites and IDPs with the NanoSIM a. Some of the X grains exhibit in SNII ejecta. Some an unusual require deep and heterogeneous mixing in pattern (enrichments Mo isotopic and 12 Presolar Grains Presolar decay of radioactive grains [15]. Among the proposed stellar sources are the proposed J-type Among C stars and born-again AGB stars. grains [15]. dredge-up. These grains aredredge-up. fro come believed to 1/2 times solar metallicity1/3 to with SiC grains [13-14]. very high 2) as well as enhanced PoS(NIC XI)021

 O is 17 Si = i  Mg. Inferred 26 - 1] x 1000. The The 1000. x - 1] O. The likely most  16 Si) O (see also section 3), O/ 28 16 18 Si/ i Silicon-isotopic compositions Si)/(

28 Si/ i [( ure 3. Fig SiC presolar different of the deviation permil in given populations from the solar ratios. solar ratios are indicated by the dashed dashed indicated by the ratios are solar lines. Data sources: [16-19, 29-30] for the for grains; C Type and unusual the [3-5]. see grains other O. These grains are likely to originate 17 distribution in AGB star grains is distribution in AGB star grains a of all grains. These grains show moderate to moderate grains show of all grains. These l grains. These grains exhibit enrichments in grains. These grains exhibit enrichments l solar positions of presolar oxides and silicates (Fig. positions of presolar oxides and silicates [33]. The Group 2 grains (~15% of all grains) The Group 2 [33]. m processing (CBP) [34] processing (CBP) [34] An was operating. m ites of the Group 4 grains are SNII ejecta (see re are the Group 3 grains, which show slight

along the SiC MS line [39-40]. This observation the SiC MS line [39-40]. along ded into distinct groups [31-32]. Most abundant Most abundant ded into distinct groups [31-32]. O, except for one grain in which com 5 dredge-up of s-process Si occurred. may of s-process have dredge-up 17 ho propose an origin from the winds of post-AGB an origin from ho propose for Group 1, 3, and 4 grains; Group 2 grains tend to to 2 grains tend Group grains; and 4 1, 3, for Group -2 ) to 0.2, which The result of CBP [32]. be the may Si- -3 ‰ ( to 10 -4 Si AGB stars of about solar Because inmetallicity. stars 30  O and moderately in enriched 18 O and close to solar or slightly solar lower than 17 Al ratios from 10 B 27 O. Possible stellar sources include low-metallicity, low-mass AGB stars and O, possibly pointing to origins [32, 38]. 38]. [32, nova origins to pointing O, possibly 16 17 Mainstream Type A&B Type Y&Z Type X Nova Unus./Type C Peter Hoppe Peter Al/ Presolar SiC 26 O ratio depends mainly on stellar mainlymass,on its O ratio depends -1000 0 1000 2000 3000 4000 0 16 Al ratios are typicallyAl ratios 10 O/ 4000 3000 2000 1000 Many but not all presolar oxide and silicate grains carry silicate oxide and radiogenic all presolar not Many but A large data set exists on the O-isotopic A large data set exists on the O-isotopic -1000 27 17 Al/ O and slight to moderate enrichments to O and slight in moderate alternative explanation is given by [35] alternative explanationw is given by [35] inenrichments from low-massfrom AGB starswhich cool botto in stars and planetary nuclei. Relatively ra stellar sources are 1.2-2.2 M stellar sources 1.2-2.2 are 26 18 sensitive measure of the mass distribution of the parent stars. The upper mass limitM of 2.2 parent stars. The upper mass distribution of the of the mass sensitive measure Presolar Grains Presolar section 3). Only two grains have been found with strong enrichments in with strong enrichments have been found section 3). Only two grains strongly depleted [36]. The s favoured formation strongly[36]. depleted isotopic compositions of presolar silicates plot presolar silicates isotopic compositions of confirms the GCE interpretation the SiC MS line of because O-rich grains form early in the AGB starsor only little evolution of when no the expected predominant signature of SN grains [37]. A few grains show very [37]. strong signature of SN grains the expected predominant inenrichments has been inferred from a comparison of the grain data with the results fromhas been inferred from a comparison grain of the a Monte Carlo IMF was assumedwhich a Salpeter simulation in in depleted are strongly the have higher SNe. The Groupgrains make up about 10% of al 4 4). Similar to SiC, presolar O-rich dust is divi 4). Similar about 70% comprise are the Group 1 grains, which large enrichments in PoS(NIC XI)021 Si 29 Si has Si has Si rate, 30 29 ,n)  Ti in grain “B” Si and Si and Ti-rich grain; for for grain; Ti-rich ed lines. “Gr. 4, lines. “Gr. ed 48 44 29 Mg( 26 Ti/ 44 Si; these grains have beenSi; is has also implications for -isotopic compositions compositions Oxygen-isotopic 30 Si [11]. With the modified Si [11]. 29 The Si in these grains is clearly Si ratio of two times the solar ratio two times of Si ratio Si can be largely [18]. resolved 30 the other grains [32, 39, 41] and and 41] 39, [32, grains other the [3-5]. in references Figure 4. oxide presolar of groups different of the ratios are solar grains. The and silicate by the dash indicated MEI”: Group 4 grains, multi-element isotopeData sources: data; Gr. [32] for the for [38] 4, MEI, 29 Si/ 29 adjustment to SN models it is possible to to SN models adjustment II origin is clearly favoured. Heavy Si is Heavy is Si clearly favoured. is origin II s in recent years which have advanced our ssible to extend the isotope studies to sub- ssible to extend the isotope studies d sufficient Si from these to zones is d sufficient mixed , it is possible to account for the observed Si- large contributions from the O/Ne zone. It was

e andnew insights into SN which gave 6 [16-19, 29-30]. 29-30]. [16-19, Si and depletions in Si yield in the O/Si and O/Ne zones is two times 29 29 of the currently used rate. Th Si yield can be achieved bySi a 3x higher 29 grains has a very high very high grains has a m-sized SiC grain with strong enrichments in  Peter Hoppe Peter recentlyonly one

In the following I will discuss selecteddiscuss In the following I will finding yield the discrepancy predicted and observed between distinct from that in AGB star and nova grains. It is also distinct from that in the SN X It is also distinct from distinct from that in AGB star and nova grains. grains; however, a large range of Si-isotopic SNII compositions is possible in ejecta if and a SN matter from different layers is mixed found in the O-rich zones (Fig. 5) and, provide the O-rich zones found in (Fig. 5) and, the sites in the ejecta where SiC grains form isotopic signatures. One of the unusual/Type C (grain “B” in relative Fig. 3). This implies originally proposed by that the [42] simultaneously account for the C- and Si-isotopic ratios as well as the the C- and Si-isotopic account for simultaneously higher than currently predicted and only with this higher than currently predicted been found. With the NanoSIMS it became po With the NanoSIMS it became been found. micrometer-sized grains and this revealed several SiC grains with very heavySi as well as two grains with in enrichments large which is within the uncertainties GCE of 2) (i.e, a factor waywhich predict models too little named “unusual” or “Type C” (Fig. 3) named [18]. A twofold increase of the Until

understanding of presolar grains from SN understanding nucleosynthesis, chemistry, and dust formation. and dust formation. chemistry, nucleosynthesis, 2. 3. Recent advances Presolar Grains Presolar 1. PoS(NIC XI)021

 Fe Si, 56 28 Si/ Fe/ Fe with 30 57 f solar- f 57 O, O, 16 O/ model of [46]. of [46]. model Fe, and 18  56 Profiles o Fe/ 54 S, 32 S/ Fe and one would expect to find expect Fe and one would Figure 5. 34 normalized SNII [45]. The different SN layers layers SN different The [45]. SNII the top. are indicated at ratiosof in the interior a 15 M 54 Fe ratios areFe ratios essentially normal [43]. 56 Fe and Si-isotopic ratios of X grains by grains by X of ratios Si-isotopic and Fe i/S zones (Fig. 5). However, the normal (Fig. 5). However, the normal zones i/S Fe/ chemistry. supported is also This idea by 56 54 letions of the heavy in two SiC isotopes) r a SN origin of these grains. Clearr a SN origin evidence agreement between the O, Mg, and/or Ca the O, Mg, and/or between agreement O enrichments are theO enrichments of result of admixture Fe/ ns was debated for a long time and among the and among a long time ns was debated for 18 57

7 SNII mixing models. In these models In these SNII most models mixingmatter models.  O enrichments. Its O- and Mg-isotopic compositions as 16 Ca ratio of ~60x solar, has now also been found for an extremely for has now also been found Ca ratio of ~60x solar, 40 Ca/ 44 Ti at the time of grain formation in presolar SiC X and low-density SiC X and presolar in formation time of grain at the Ti 44 Ti ratio can be well explained in the context of the 15 M context of the ratio can be well explained in the Ti 48 Ti/ Fe in X grains. It is possible to overcome this problem if Fe from the outer He/C Fe from if is possible to overcome Fe in X grains. It this problem Peter Hoppe Peter 44 54 Fe is puzzeling since the Si/S zone is veryFe is puzzeling since rich in Fe of up to 2x the solar ratio; in contrast, to 2x the solar ratio; Fe of up Ti, based on a Ti, 56 56 44 O-enriched spinel grain (Fig. 4) [38]. This finding strongly supports the proposed SN proposed the strongly supports This finding (Fig. 4) [38]. spinel grain O-enriched Fe/ Fe/ comes from the H and He/N zones and the mixing SNII matter from themixing SNII He/N, He/C, and S 16 54 57 enhanced matter from the Mg a SNII origin comes from support for He/C zone (Fig. 5). Additional 44]. grains [40, and Si isotope data of Group 4 silicate origin of the veryorigin of the rare grains with It is possible to simultaneously explain the It is possible graphite grains has been taken as final proof fo for well as its SiC X grains contain up to 0.5 wt% Fe. Most X grains exhibit enrichments in enrichments X grains exhibit Fe. Most to 0.5 wt% contain up SiC X grains the recent finding of S isotope anomalies (dep the recent finding [17-18]. Si isotopes enrichments in the heavy grains with strong the Group 4 oxide/silicate grai The origin of and He/N zones would have been preferentially trapped, e.g., due to element fractionation to element due e.g., been preferentially trapped, have and He/N zones would between from different zones bymatter proposed stellar sources were SNeII and high-metallicity stars. AGB From multi-element clearly now origin is grains (cf. Fig. 4) the SNII oxide isotope data for three Group 4 is based on the excellent This favoured [32]. isotope data and predictions from 15 M from isotope data and predictions The presence of

Presolar Grains Presolar 3. 4. 5. PoS(NIC XI)021

.  Cr 54 , , Nature (2008)138 43.

Al ratios than SiC Al ratios 27 Al/ 26 n n stellar nucleosynthesis Space Sci. Rev. Sci. Space , , Elsevier, Amsterdam 2007. 2007. Amsterdam , Elsevier, Interstellar diamonds in meteorites O excesses? The intermediate O-rich Carbon, ,Carbon, magnesium, silicon and 16 can be explained, at least qualitatively, can be explained, Cr variations on a Cr variations macroscopic scale and it 54 e fact that the parent stars of SiC follow the e fact that the parent stars of SiC odel predictionsis based on ad-hoc mixing ith the inferences from the presolar grain data. <200 nm-sized with large oxide grains been used to constrai onsider the physics of mixing and molecule and molecule onsider the physics of mixing

to shed more light on this issue. 8 are expected to contribute significantlyto the inter- Al ratios of O-rich grains but not for the Al-isotopic Al-isotopic the for not but O-rich grains Al ratios of  27 Al/ unsolved problems, e.g., the following: unsolved problems, (2005) 93. 26 O-rich and one would expect to find much more of these one would expect to find much O-rich and 65

16 (1994)430 870. Meteorites,and Comets, Planets r, T. Ireland,S. Lewis, R.

O excesses. 18 , ApJ Presolar grainsmeteorites: early thePresolar times of Remnants from from the Evidence forSiCMurray interstellar in the carbonaceous meteorite , et al. , Chemie der Erde – I wish to thank the organizers of the Nuclei in the Cosmos XI conference for the the for conference XI Cosmos the in Nuclei of the organizers the thank to wish I – Reservoir for Material: Circumstellar Grains Material: Circumstellar for Comet Reservoir Peter Hoppe Peter 326 (1987)160. Nature titanium isotopic compositions of single interstellar siliconcarbide grainsfrom Murchison the carbonaceous solar system solar (1987)330 728.

ny of the isotopic properties of presolar grains Many of the ratios in SiC from AGB stars. A better understanding of the role of CBP in the evolution of of evolution of CBP in the role of the AGB stars. A better understanding from ratios in SiC stars may help low- and intermediate-mass Why only are there so few SN grains with large stellar dust inventory [49] w which is at odds stellar dust inventory [49] stars tend to have higher AGB grains from Presolar oxide/silicate zones in SNII are extremely enrichments have been found [47-48]. likelyThe most grains are SNeII, in sources of these enrichments have been found [47-48]. and O/Cparticular the O/Ne zones (see et al. in this issue). also the contribution by Nittler was speculated that these variations are caused by different amounts of Cr-bearing of are that these variations was speculated presolar caused by amounts different Just recently, planetary grains in matter. grains [50]. This is surprising in view of th view in This is surprising grains [50]. parent stars is processing of O-rich dust in their evolutionary sequence. Cool bottom high the account for required to The comparison of SN grain data with m calculations. More realistic that c models chemistry are clearly needed. grains than SN grains with grains than SN AGB star grains appear to come largely stars with from masses between 1.2 and 3 M It is known since long that meteorites show since long that It is known meteorites However, AGB stars heavier than 4 M

[3] P. Hoppe, [3] P. [4] [4] Amari, S. K. Lodders, [6] P. Hoppe, S. Amari, E. Zinne [5] [5] in Grains, E. Presolar Zinner, [2] [2] E. Steel, Anders, E. Wacker, F. J. Tang, M. Lewis, R. S. [1] T. Bernatowicz T. [1] 3. models and mixing conditions in SN ejecta, which has openened a new window to astrophysics. astrophysics. to a new window has openened which SN ejecta, in mixing conditions and models Nevertheless, there are still numerous 2. 4. Acknowledgements invitationpresent to paper. this References 1. Unsolved problems 4. Unsolved problems Presolar Grains Presolar 6. by stellar have The presolar grain data models. PoS(NIC XI)021

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