Late Injection of Radionuclides Into Solar Nebula Analogs in Orion

Lunar and Planetary Science XXXV (2004) 2116.pdf LATE INJECTION OF RADIONUCLIDES INTO SOLAR NEBULA ANALOGS IN ORION. N. Ouellette and S.J. Desch, Dept. Physics and Astronomy, Arizona State University, Tempe, AZ 85287 ([email protected]). Recent evidence for live 60Fe in the early solar structure until the passage of the supernova shock. system [1,2] clearly indicates that the solar system The timescale for the shock to reach the proplyd, formed near a supernova, in a region of high-mass using 2000 km s−1 from the supernova remnant Cas star formation. Except for 10Be, which has a sep- A as a typical ejecta velocity [9], is a few decades. arate, unique origin in galactic cosmic rays [3], it When the ejecta strikes the proplyd, a shock is gen- appears likely that many of the other short-lived erated that penetrates deeper into the proplyd until radionuclides could be produced in their correct a maximum density is reached, when the ram pres- proportions in a type II supernova explosion. It sure behind the shock equals the gas pressure in is natural, then, to study proplyds (photoevapo- the proplyd. For the energy budget of a supernova 3 rating disks ∼ 10 AU across [4]) and the smaller like Cas A (progenitor mass ∼ 15 M [9]), and as- protoplanetary disks observed in the Orion Nebula suming an expansion of the supernova explosion to [5] as analogs to our own solar system. These disks about 1017 cm, the ram pressure behind the shock is and proplyds tend to reside at small distances, ∼ ∼ 0.3 erg cm−3. Thus the shock will penetrate until a few ×1017 cm from the central stars of the Orion it reaches densities ∼ 3 × 10−12 g cm−3. Supernova Nebula, especially the O6 star θ1Ori C [4]. This shocks can propagate until they are very deep in ∼ 40 M star will supernova in the next few Myr, the photoevaporative flow, stalling only when the and when it does, the solar nebula analogs in the almost reach the protoplanetary disk itself. For ex- Orion Nebula will lie in the path of the ejecta. ample, a disk with ρ ≈ 10−9 g cm−3 at the mid- This ejecta is sure to contain many of the short- plane at 1 AU will have ρ < 10−12 g cm−3 only 1 lived radionuclides known to have been extant in AU above the disk, assuming a 0.1 AU scale height. the early solar system, including 26Al, 60Fe, 41Ca, Radionuclides such as 26Al and 60Fe in super- 36 and Cl [6]. In this abstract we assess the likeli- nova ejecta will condense out as dust grains of Al2O3, hood that protoplanetary disks in the Orion nebula Fe3O3 MgSiO3 and SiC, in a matter of months to could intercept and incorporate short-lived radionu- a year in the case of SN1987A [10,11]. Presolar clides from a nearby supernova. We consider the SiC grains associated with formation in supernova physical form in which the radionuclides exist, the ejecta have been found in meteorites and their sizes trajectories taken by the ejecta, and the timing of tend to follow a log-normal distribution, centered their injection. We then compare our predictions on a radius ∼ 0.5 µm [12,13] to our own solar system to assess whether the solar We have calculated the trajectories of these radio- system formed in an Orion-like setting. nuclide bearing dust grains as the ejecta they are The proplyds in Orion are disks that have al- in collides with proplyds or protoplanetary disks. If ready formed. Irradiation by the EUV and FUV the dust grains are in the leading edge of the ejecta, fluxes from the central O stars, especially θ1Ori C, they will separate from the shock front as it begins heats the gas in the disk to ∼ 1000 K, causing the to stall as it passes through the photoevaporative gas to expand and driving an outflow of neutral gas flow. We have modeled the density and velocity away from the disk. The hydrodynamics of this flow structure of the outflow according to [1], and we have been modeled and found to be in good agree- have calculated the drag forces and frictional heat- ment with observations [4]. The outflow extends ing of dust grains passing through it. We assume outward for several hundred AU, and is character- an initial dust velocity of 2000km−1 s−1 . Table I ized by densities ρ ∼ 10−19 − 10−18 g cm−3. This shows the results for dust passing through an EUV- stage lasts for several ×104 yr to 1 × 105 yr, after dominated outflow, indicating the radius of the dust which the disk has lost considerable mass due to particle,the peak temperature of the dust grain, evaporation. and whether or not it successfully passed through If a nearby supernova explodes while the pro- the photoevaporative flow into the protoplanetary plyd is still photoevaporating, the flow is hardly disk. From these results we see that a photoevap- disturbed by the extra radiation. As in the case of orative flow acts as a cushion, allowing supernova SN1987A, UV fluxes typically drop in a year or less grains to enter the protoplanetary disk intact. [7,8], and the flow quickly returns to its previous Without this cushion, we find that radionuclide- Lunar and Planetary Science XXXV (2004) 2116.pdf Table 1 Dust injection in a PDR region 26 −19 −3 dionuclides like Al [17]. One caveat is that the r ∼ 250 AU, ρ ∼ 5 × 10 g cm prompt injection (in < 102 yr) of radionuclides into the solar system does not allow 41Ca time to decay, dust radius Tmax injected? 41 µm K and would lead to an overabundance of Ca in the 10 250 yes early solar system [6]. This problem may be amelio- 1 250 yes rated, however, if the supernova ejecta was spatially 0.1 250 no highly inhomogenous, as is observed in the Cas A supernova remnant [9]. Nevertheless, simple inte- gration of the initial mass function indicates that bearing dust grains can penetrate the shock front, over 85 % of solar-type stars did form in environ- but then quickly evaporate as they encounter much ments like Orion, containing at least one star mas- denser gas on the other side. While such grains sive enough to supernova [18]. In future work we would not survive intact, they would nonetheless plan to further explore these issues in greater quan- contribute their radionuclides to the protoplane- titative detail to assess whether our Sun was one of tary disk. Given that the photoevaporating pro- those 85 %, and whether it acquired its short-lived 5 plyd stage lasts for at most 10 years, while the radionuclides by formation in proximity to a super- lifetime of the Orion Nebula is ∼ 1 Myr, it is un- nova. likely that a given disk will be photoevaporating when the supernova explodes. We view injection of References: [1] Tachibana S & Huss G 2003, ApJ radionuclides borne by dust grains as a likely event, 588, 41 [2] Mostefaoui S, Hoppe P, Marhas KK & but not without the destruction of those dust grains Groner E 2003, MPSA 38, 5185 [3] Desch SJ, Con- as they enter the protoplanetary disk. nolly HC Jr & Srinivasan G 2004, ApJ, in press We now consider the likely amounts of radioac- [4] Johnstone D, Hollenback D & Bally J 1998, ApJ tivities that would be injected into a protoplanetary 499, 758. [5] McCaughrean, MJ & O’Dell, CR 1996, AJ 111, 1977 [6] Meyer BS, Clayton DD, The LS disk in Orion. The explosion of a 25 M star in a −5 26 & El Eid MF 2003, LPSC 34, 2074 [7] Hamuy M type II supernova ejects about 7 × 10 M of Al [14], and the number of 26Al atoms intercepted at & Suntzeff NB 1990, AJ 99, 1146. [8] Walker AR a distance 1017 cm from the supernova would be & Suntzeff NB 1991, PASP 103, 953. [9] Willingale about 5 × 1016 (A/cm2), where A is the disk area. R et al 2003, A&A 398, 1021 [10] Douvion T, La- The solar system contains about 1018 (M/g) 27Al gage PO & Pantin E 2001, A&A 369, 589. [11] atoms [15], where M is the disk mass. Taking the Kozasa T, Hasegawa H & Nomoto K 1991, A&A column density M/A at 3 AU to be ∼ 103 g cm−3 249, 474. [12] Hoppe P et al 2000, MPS 35, 1157. [16], we find a 26Al/27Al ratio ∼ 5×10−5. We there- [13] Amari S et al 1994, Geochemica et Cosmochem- fore conclude that it is reasonable for the solar sys- ica Acta 58, 459. [14] Woosley SE & Weaver TA tem to have acquired its short-lived radionuclides 1995, ApJss 101, 181. [15] Anders E & Grevisse N in this fashion if it formed in an Orion-like setting. 1989, Geochemica et Cosmochemica Acta 53, 197. This scenario has the added advantage of provid- [16] Hayashi, C, Nakagawa, K & Nakazawa K, PP ing a late injection of 26Al into the solar system, II (U of A), p. 1100 [17] Sahijpal, S & Goswami, JN explaining why FUN inclusions appear depleted in (1998) ApJL 509, L137 [18] Adams FC & Laughlin neutron-rich stable isotopes and in short-lived ra- G 2001 Icarus 150, 151.

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