beyond the agb
DESCRIPTION
Beyond the AGB. My new E-mail: [email protected]. ( 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. - PowerPoint PPT PresentationTRANSCRIPT
Stellar model
Inputs: opacity, eos, neutrinos rate,
thermonuclear rates…..
Outputs: Luminosity, effective temperature, chemical
composition…..
Sometime, ba-stards 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.)
Radiation LNGS/surface
muonsneutronsPhotons
10-6
10-3
0.2
Laboratory for Underground Nuclear Astrophysics
The adopted set-upThe adopted set-up
SPECIFICATIONS
Umax= 50 – 400 kV
I 500 A for proton
Emax= 0.07 keV
The H burning The H burning
p + p 2H + e+ + [0.27 MeV] p + e- + p 2H + e+ + [1.44 MeV]
2H + p 3He +
3He + 3He 4He + 2p 3He + 4He 7Be + 3He + p 4He + e+ +
7Be + e- 7Li + [0.81 MeV] 7Be + p 8B +
7Li + p 8Be 8B 8Be + e+ + [6.80 MeV]
8Be 2 4He 8Be 2 4He
99.75%99.75% 0.25%0.25%
86%86% 14%14%
99.89%99.89% 0.11%0.11%
CHAIN IIICHAIN IIIQQeffeff= 19.67 MeV= 19.67 MeV
CHAIN II CHAIN II QQeffeff= 25.66 MeV= 25.66 MeV
CHAIN ICHAIN IQQeff eff = 26.20 MeV= 26.20 MeV
CHAIN IVCHAIN IVQQeffeff= 16.84 MeV= 16.84 MeV
pp chain
22··1010-5-5%%
LUNA 2001
LUNA 1999
NABONA 2000 & LUNA 2001
ERNA & LUNA
NABONA
0E+00
2E+00
4E+00
6E+00
8E+00
1E+01
0 50 100 150 200 250 300 350 400
E (keV)
S-f
acto
r (k
eVb)
solid target tot
gas-target
14N(p,)15O: the bottleneck of the CNO
Stellar Energies: the Gamow’s peak
Isochrones for Globular ClustersIsochrones for Globular Clusters
Imbriani, Costantini, Formicola et al. , A&A, 420, 2004
The age of the oldest Globular Clusters should be The age of the oldest Globular Clusters should be increased by about 0.7-1 Gyrincreased by about 0.7-1 Gyr
V - I
Straniero et al. 1999
from
VI TORINO WORKSHOP
ROMEEd. by Franca
D’Antona
Further Adventures
• 12C()16O @ ERNA
• 25Mg(p,)26Al @ LUNA
Coming soon
M-R relation:high rate = shorter C burning =
more compact
progenitorEnd of C-burning
Onset of core collapse
Beginning of Ne-burning
From Imbriani et al. 2001 ApJ 558,903
YieldsAffected 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
AMICAAntarctic 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.
Top 25 - 35 K
Top 4 - 10 K
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)
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
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
2nd stage: 0.8 W @ 4.2 K1st stage: 35 W @ 41 KMin temp.: 0 W @ 2.8 KType: GMCooling: 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
Riunione IRAIT-AMICA
Roma, 27 Gennaio 2006
IMPORTANTE: Serie di cryocooler già sperimentati in Antartide.
Riunione IRAIT-AMICA
Roma, 27 Gennaio 2006
Taormina, June, 2005
The AMICA Control System:
TEMP- CONTROLLEDAMBI ENT
-10 c° / 10 c°
AMICACRYOSTAT
- 40 c° / - 80 c°external temperature
NIRPRE-AMPCLOCK
BOX
MIRPRE-AMPCLOCK
BOX4.2 K40 K
cryo-cooler CRYO-COOLERCOMPRESSOR
DUAL-STAGESTEP-MOTORCONTROLLER
VACUUMPUMP
VACUUMCOMMANDED
VALVEP-GAUGE
TEMPERATURE&
STEP-MOTORCONTROL
TEMP- CONTROLLEDAMBI ENT
-10 c° / 10 c°
C-PCI CRATEHOST PENTIUM CPU
NIR/MIR DETECTORCONTROLLER
LAKESHORETEMPERATURE
CONTROLLER & MONITOR
CONTROLPLC
PMC DETECTORCONTROL I/F
An Example
Source Flux : 9.5 JyIntegration time : 20 s (0.01s x frame)Point source overall counts (ADU): 5.88154e+006Point source clean counts (ADU): 1.79103e+006Sky average counts (ADU): 83479.9Signal-to-noise ratio: 20.4989
λ : 21 μ
Riunione IRAIT-AMICA
Roma, 27 Gennaio 2006
http://www.te.astro.it/attivitascientifica/progetti/amica/index.htm