Beyond the AGB (not in the sense of stellar evolution) My new

Stellar model Inputs: opacity, eos, neutrinos rate, thermonuclear rates….. Outputs: Luminosity, effective temperature, chemical composition…..

Sometime, ba-star d s are lucky Lab for Underground Nuclear Astrophysics (LUNA) Ba-star-dini head quarter Gran Sasso Sn Watch-dog IR Telescope (SWIRT)

Noise reduction at LNGS (shielding: 4000 m w.e.) RadiationLNGS/surface muons neutrons Photons Laboratory for Underground Nuclear Astrophysics

The adopted set-up SPECIFICATIONS U max = 50 – 400 kV I  500  A for proton  E max = 0.07 keV

The H burning  p + p  2 H + e + + [0.27 MeV] p + e - + p  2 H + e + +  [1.44 MeV] 2 H + p  3 He +  3 He + 3 He  4 He + 2p 3 He + 4 He  7 Be +  3 He + p  4 He + e Be + e -  7 Li + [0.81 MeV] 7 Be + p  8 B +  7 Li + p  8 Be 8 B  8 Be + e + + [6.80 MeV] 8 Be  2 4 He 8 Be  2 4 He 99.75%0.25% 86%14% 99.89%0.11% CHAIN III Q eff = MeV CHAIN II Q eff = MeV CHAIN I Q eff = MeV CHAIN IV Q eff = MeV pp chain 2·10 -5 % LUNA 2001 LUNA 1999 NABONA 2000 & LUNA 2001 ERNA & LUNA NABONA

14 N(p,  ) 15 O: the bottleneck of the CNO

Stellar Energies: the Gamow’s peak

Isochrones for Globular Clusters Imbriani, Costantini, Formicola et al., A&A, 420, 2004 The age of the oldest Globular Clusters should be increased by about Gyr V - I

Straniero et al from VI TORINO WORKSHOP ROME Ed. by Franca D’Antona

Further Adventures 12 C(  ) 16 ERNA 25 Mg(p,  ) 26 LUNA Coming soon

M-R relation: high rate = shorter C burning = more compact progenitor End of C- burning Onset of core collapse Beginning of Ne- burning From Imbriani et al ApJ 558,903

Yields Affected by the steepness M-R relation Affected by the amount of C available for shell burning

NOW, ON THE TOP …. and ON THE ICE

CW-Leo: a red lighthouse Reflected V light Irradiated IR light (10  m 

Stardust Grain signatures are more clear above 3  SiC grains

Courtesy of Busso & Co

The IRAIT project, a Italian-Spanish collaboration

CONCORDIA (3200 m)

The Robotic Telescope

Riunione IRAIT-AMICA Roma, 27 Gennaio 2006 AMICA Antarctic Multiband Infrared CAmera

I due rivelatori di AMICA SWA (1-5  m) Array InSb 256 x 256 Raytheon Corp. LWA (5-28  m) Array Si:As BIB MF-128 DRS Techn. Inc. T op  K T op  K Riunione IRAIT-AMICA Roma, 27 Gennaio 2006

entrance window LWA SWA folding mirror exit pupil collimator mirror camera mirror sliding mirror 330 mm 150 mm Riunione IRAIT-AMICA Roma, 27 Gennaio 2006

Sistema ottico di AMICA Sistema completamente riflettente 4 specchi dorati (2 parabole fuori asse + 2 piani) Riduttore di focale 1 : 1.47 Diffraction-limited performances Campionamento ottimale PSF di Airy a 3  m su SWA e a 10  m su LWA Scala:0.538 arcsec / pix (SWA) arcsec / pix(LWA) FOV:2.29  2.29 arcmin 2 (SWA) 2.87  2.87 arcmin 2 (LWA) Riunione IRAIT-AMICA Roma, 27 Gennaio 2006

Finestra d’ingresso e filtri Finestra in CdTe ad alta trasmissione (>70 % tra 1 e 25  m) Filtri in quarzo ( 13  m): Banda larga 2.21  m (0.34  m) 3.43  m (0.60  m) 5.08  m (0.39  m) 8.79  m (0.98  m)  m (3.29  m)  m (3.40  m)  m (1.95  m) Banda stretta 3 filtri eventuali da scegliere da una lista già compilata Riunione IRAIT-AMICA Roma, 27 Gennaio 2006 Finestra d’ingresso realizzata insieme al criostato da IRlabs. Contatti in corso con Barr Associates per i dettagli dei filtri.

ARS Displex Closed Cycle Cryocooler DE-210S with ARS-10 Compressor 2 nd stage: K 1 st stage: K Min temp.: K Type: GM Cooling: Water, CUSTOM Power consumption: V AC, 3 phase, 50 Hz Ambient temperature range: 5 to 35°C Cooling water: Minimum flow 8 27°C maximum temperature Riunione IRAIT-AMICA Roma, 27 Gennaio 2006 IMPORTANTE: Serie di cryocooler già sperimentati in Antartide.

Riunione IRAIT-AMICA Roma, 27 Gennaio 2006

An Example Riunione IRAIT-AMICA Roma, 27 Gennaio 2006