1 / 34

Beyond the AGB

Beyond the AGB. My new E-mail: oscar.straniero@bastardini.com. ( not in the sense of stellar evolution ). Inputs: opacity, eos, neutrinos rate, thermonuclear rates…. Outputs: Luminosity, effective temperature, chemical composition…. Stellar model. Ba-star-dini head quarter.

ronnie
Download Presentation

Beyond the AGB

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Beyond the AGB My new E-mail: oscar.straniero@bastardini.com (not in the sense of stellar evolution)

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

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

  4. Laboratory for Underground Nuclear Astrophysics Noise reduction at LNGS (shielding: 4000 m w.e.)

  5. The adopted set-up SPECIFICATIONS • Umax= 50 – 400 kV • I 500 mA for proton • DEmax= 0.07 keV

  6. The H burning pp chain p + p  2H + e+ +n[0.27 MeV]p + e- + p  2H + e+ +n [1.44 MeV] 2H + p  3He +g 3He + 3He  4He + 2p 3He + 4He  7Be +g 3He + p  4He +e+ +n 7Be + e-  7Li +n[0.81 MeV]7Be + p  8B +g 7Li + p  8Be 8B  8Be + e+ +n[6.80 MeV] 8Be  2 4He8Be  2 4He 99.75% 0.25% LUNA 2001 2·10-5% 86% 14% LUNA 1999 ERNA & LUNA 99.89% 0.11% NABONA NABONA 2000 & LUNA 2001 CHAIN II Qeff= 25.66 MeV CHAIN I Qeff = 26.20 MeV CHAIN III Qeff= 19.67 MeV CHAIN IV Qeff= 16.84 MeV

  7. 14N(p,g)15O: the bottleneck of the CNO

  8. Stellar Energies: the Gamow’s peak

  9. Isochrones for Globular Clusters The age of the oldest Globular Clusters should be increased by about 0.7-1 Gyr V - I Imbriani, Costantini, Formicola et al., A&A, 420, 2004

  10. Straniero et al. 1999 from VI TORINO WORKSHOP ROME Ed. by Franca D’Antona

  11. Further Adventures • 12C(a,g)16O @ ERNA • 25Mg(p,g)26Al @ LUNA Coming soon

  12. End of C-burning From Imbriani et al. 2001 ApJ 558,903 M-R relation:high rate = shorter C burning = more compact progenitor Onset of core collapse Beginning of Ne-burning

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

  14. NOW, ON THE TOP …. and ON THE ICE

  15. Irradiated IR light(10 mm) CW-Leo: a red lighthouse Reflected V light

  16. SiC grains Stardust Grain signatures are more clear above 3 m

  17. Courtesy of Busso & Co

  18. The IRAIT project, a Italian-Spanish collaboration

  19. CONCORDIA (3200 m)

  20. The Robotic Telescope

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

  22. Riunione IRAIT-AMICA Roma, 27 Gennaio 2006 I due rivelatori di AMICA Array InSb 256 x 256 Raytheon Corp. SWA (1-5 m) Top  25 - 35 K Array Si:As BIB MF-128 DRS Techn. Inc. LWA (5-28 m) Top  4 - 10 K

  23. 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) 1.345 arcsec / pix (LWA) •FOV: 2.29  2.29 arcmin2 (SWA) 2.87  2.87 arcmin2 (LWA)

  24. 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 (<6 m), germanio (6 m<<13 m) e CdTe (>13 m): Banda larga K @ 2.21 m (0.34 m) L @ 3.43 m (0.60 m) M @ 5.08 m (0.39 m) N1 @ 8.79 m (0.98 m) N2 @ 11.63 m (3.29 m) Q1 @ 18.96 m(3.40 m) Q2 @ 22.40 m (1.95 m) Banda stretta 3 filtri eventuali da scegliere da una lista già compilata Finestra d’ingresso realizzata insieme al criostato da IRlabs. Contatti in corso con Barr Associates per i dettagli dei filtri.

  25. Riunione IRAIT-AMICA Roma, 27 Gennaio 2006 ARS Displex Closed Cycle Cryocooler DE-210S with ARS-10 Compressor 2nd stage: 0.8 W @ 4.2 K 1st stage: 35 W @ 41 K Min temp.: 0 W @ 2.8 K Type: GM Cooling: Water, CUSTOM Power consumption: 6 kW @ 200 V AC, 3 phase, 50 Hz Ambient temperature range: 5 to 35°C Cooling water: Minimum flow 8 LPM @ 27°C maximum temperature IMPORTANTE: Serie di cryocooler già sperimentati in Antartide.

  26. Riunione IRAIT-AMICA Roma, 27 Gennaio 2006

  27. Riunione IRAIT-AMICA Roma, 27 Gennaio 2006 An Example

  28. http://www.te.astro.it/attivitascientifica/progetti/amica/index.htmhttp://www.te.astro.it/attivitascientifica/progetti/amica/index.htm

More Related