Old pre-main-sequence stars
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1 Old pre-main-sequence stars and a second chance for planet formation Peter Scicluna Uni Kiel & ESO, Garching 9th September 2014 Giovanni Rosotti (MPE, USM, IoA) Leonardo Testi (ESO, INAF) Jim Dale (Excellence Cluster Universe) A&A, 566, L3 Peter Scicluna Old pre-main-sequence stars 9th September / 14
2 Star formation + discs Stars form in collapsing clouds Residual angular momentum disc formation Disc observed indirectly through 1 IR Excess (stellar flux reprocessed by dust disc) 2 UV Excess & Spectral lines (accretion region) Isella (2006) Peter Scicluna Old pre-main-sequence stars 9th September / 14
3 Timescales - Disc dissipation τ disc 2 3 Myr (Caution: Bell et al. (2013) suggest τ disc 5 Myr!) Strict constraint on planet formation! Fedele et al. (2010) Peter Scicluna Old pre-main-sequence stars 9th September / 14
4 Old accretors Large SFRs (Galactic, SMC, LMC) contain population of Old (> 10 Myr) accretors de Marchi et al. (2011a) Peter Scicluna Old pre-main-sequence stars 9th September / 14
5 Old accretors Large SFRs (Galactic, SMC, LMC) contain population of Old (> 10 Myr) accretors Accrete at similar rates to young PMS Also show NIR excess de Marchi et al. (2011b) Peter Scicluna Old pre-main-sequence stars 9th September / 14
6 Old accretors Large SFRs (Galactic, SMC, LMC) contain population of Old (> 10 Myr) accretors Accrete at similar rates to young PMS Also show NIR excess Different spatial distribution to young stars Lower X-ray luminosities old de Marchi et al. (2011a) Peter Scicluna Old pre-main-sequence stars 9th September / 14
7 Potential Solutions? Not really old? Not really accretors? Peter Scicluna Old pre-main-sequence stars 9th September / 14
8 Potential Solutions? Not really old? Not really accretors? Peter Scicluna Old pre-main-sequence stars 9th September / 14
9 Potential Solutions? Not really old? Not really accretors? Tail-end of huge population? Peter Scicluna Old pre-main-sequence stars 9th September / 14
10 Potential Solutions? Not really old? Not really accretors? Tail-end of huge population? = M init M Peter Scicluna Old pre-main-sequence stars 9th September / 14
11 Potential Solutions? Not really old? Not really accretors? Tail-end of huge population? = M init M Not the original disc? Peter Scicluna Old pre-main-sequence stars 9th September / 14
12 Bondi-Hoyle Accretion? R BH 1 v Star moves through medium Accretes material Peter Scicluna Old pre-main-sequence stars 9th September / 14
13 Bondi-Hoyle Accretion? R BH 1 v Star moves through medium Accretes material UV, lines, but no disc Peter Scicluna Old pre-main-sequence stars 9th September / 14
14 Our Model - Disc Re-formation via Bondi-Hoyle-like Accretion SFRs are clumpy Star formation happens in part of cloud Peter Scicluna Old pre-main-sequence stars 9th September / 14
15 Our Model - Disc Re-formation via Bondi-Hoyle-like Accretion SFRs are clumpy Star formation happens in part of cloud Stars disperse could enter a clump Peter Scicluna Old pre-main-sequence stars 9th September / 14
16 Our Model - Disc Re-formation via Bondi-Hoyle-like Accretion SFRs are clumpy Star formation happens in part of cloud Stars disperse could enter a clump Accrete while passing through clump Residual angular moment disc formation? Peter Scicluna Old pre-main-sequence stars 9th September / 14
17 Our Model - Disc Re-formation via Bondi-Hoyle-like Accretion SFRs are clumpy Star formation happens in part of cloud Stars disperse could enter a clump Accrete while passing through clump Residual angular moment disc formation? accretion observable for longer Peter Scicluna Old pre-main-sequence stars 9th September / 14
18 Implementation Simple Monte Carlo model, realistic SFR parameters Table: Parameters for Monte Carlo models Parameter Values f V σ v c s R cl n cl 10 2, 10 3, 10 4, km s km s pc 10 4 cm 3 Peter Scicluna Old pre-main-sequence stars 9th September / 14
19 Implementation Simple Monte Carlo model, realistic SFR parameters Probabilistic star-clump interactions Table: Parameters for Monte Carlo models Parameter f V σ v c s R cl n cl Values 10 2, 10 3, 10 4, km s km s pc 10 4 cm 3 Peter Scicluna Old pre-main-sequence stars 9th September / 14
20 Implementation Simple Monte Carlo model, realistic SFR parameters Probabilistic star-clump interactions Accretion disc, viscous evolution Table: Parameters for Monte Carlo models Parameter f V σ v c s R cl n cl Values 10 2, 10 3, 10 4, km s km s pc 10 4 cm 3 Peter Scicluna Old pre-main-sequence stars 9th September / 14
21 Implementation Simple Monte Carlo model, realistic SFR parameters Probabilistic star-clump interactions Accretion disc, viscous evolution Derive fraction of observable accretors Table: Parameters for Monte Carlo models Parameter f V σ v c s R cl n cl Values 10 2, 10 3, 10 4, km s km s pc 10 4 cm 3 Peter Scicluna Old pre-main-sequence stars 9th September / 14
22 Limitations Upper limit - Bondi-Hoyle accretion only for uniform medium Peter Scicluna Old pre-main-sequence stars 9th September / 14
23 Limitations Upper limit - Bondi-Hoyle accretion only for uniform medium Also no - clump motion - winds - magnetic fields -... Peter Scicluna Old pre-main-sequence stars 9th September / 14
24 Limitations Upper limit - Bondi-Hoyle accretion only for uniform medium Also no - clump motion - winds - magnetic fields -... f V & viscosity parameters highly uncertain Peter Scicluna Old pre-main-sequence stars 9th September / 14
25 Results Cumulative fraction f V = 10-2 f V = 10-3 f V = 10-4 f V = Accreted mass (Log (M/M O )) Fraction Accretion threshold (M O yr -1 ) significant fraction of stars re-accrete Accretion observable right numbers of Old accretors Peter Scicluna Old pre-main-sequence stars 9th September / 14
26 A Second Epoch of Planet Formation? Cumulative fraction f V = 10-2 f V = 10-3 f V = 10-4 f V = 10-5 Significant fraction accrete > 1 MMSN New planets? Different composition? Accreted mass (Log (M/M O )) Peter Scicluna Old pre-main-sequence stars 9th September / 14
27 ...or Destruction? What if planets already exist? Planet/disc interactions could - trigger migration - alter eccentricity/inclination potential chaos (Credit: James Garry, Fastlight) Peter Scicluna Old pre-main-sequence stars 9th September / 14
28 Summary Large SFRs have multiple populations of accreting stars Ages appear older than allowed in canonical model Simple model based on Bondi-Hoyle accretion qualitatively explains observations (size and distribution of populations) Potential consequences for planet formation and evolution are manifold and unpredictable Peter Scicluna Old pre-main-sequence stars 9th September / 14
29 Implementation - Monte Carlo + Viscous Evolution Draw random stars from IMF (n(m) M α, 0.7M < M < 3.2M ) Each step check for encounter with dense clump (P f V ) Calculate Ṁ BH (t) and M BH (t) Pass to viscous evolution model Simple treatment of disc formation & evolution Ṁ (t) for many stars Integrate over t to get observable fractions Table: Parameters for Monte Carlo models Parameter Values f V 10 2, 10 3, 10 4, 10 5 N stars 10 5, 10 5, 10 6, 10 7 α 2.35 σ v 1 km s 1 c s 0.3 km s 1 R cl 0.1 pc 10 4 cm 3 n cl Peter Scicluna Old pre-main-sequence stars 9th September / 14
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