1993.1

Metal-deficient, H- and He-burning  structures.
 

Evolutionary tracks Z=1.0E-10 - Y=0.23 (0.6-15)Mo

Evolutionary tracks Z=1.0E-6 - Y=0.23 (0.6-15)Mo

Evolutionary tracks Z=1.0E-4 - Y=0.23 (0.6-6)Mo

Note 1: Lower masses till the He flash, larger masses till the C ignition.
Note 2: HB in 1996

Ref: Cassisi S. & Castellani V. , ApJS, 88, 509

1994.1

Metal poor, H- and He-burning  structures.
 

Evolutionary tracks Z=1.0E-3 - Y=0.23 (0.6-9)Mo	Evolutionary tracks Z=6.0E-3 - Y=0.23 (0.6-9)Mo
Evolutionary tracks Z=1.0E-3 - Y=0.27 (0.6-9)Mo	Evolutionary tracks Z=6.0E-3 - Y=0.27 (0.6-9)Mo

Ref: Cassisi S., Castellani V. & Straniero O., A&A, 282, 753

1995.1

Metal poor, H- and He-burning, low- and intermediate mass stars

Readme
 

Z=0.0001 Y=0.230 - standard - ml=1.6	H-burning models  (0.6 - 2.2)Mo	He burning models (1.0 - 2.0)Mo	isochrones (0.5-15) Gyr
Z=0.0004 Y=0.230 - standard - ml=1.6	H-burning models  (0.75 - 2.0)Mo	He burning models (1.0 - 2.0)Mo	isochrones (1.0-10) Gyr

Note 1: Standard = no diffusion; ml = mixing length

 Ref: Castellani V. & Degl'Innocenti S., A&A,  298, 827

1996.1

Metal-deficient He-burning  (HB) structures.
 

Evolutionary tracks Z=1.0E-10 - Y=0.23

Evolutionary tracks Z=1.0E-6- Y=0.23

Evolutionary tracks Z=1.0E-5 - Y=0.23

Note 1:  For two choices on the mass of the RGB progenitor (0.8 or 1.0 Mo). i.e. on the cluster age.
 

H burning phases.
 

Isochrones Z=1.0E-10 - Y=0.23 (3-20)Gyr

Isochrones Z=1.0E-6 - Y=0.23 (3-20)Gyr

Isochrones Z=1.0E-5 - Y=0.23  (3-20)Gyr

 Ref: Cassisi S., Castellani V. & Tornambe' A., ApJ, 459, 298

1997.1

Not-too-old metal-deficient structures  Z=1.0E-5 - Y=0.23
 

H burning tracks (0.6-2.2)Mo

Horizontal Branch tracks RGB progenitors: (1.0-1.8)Mo

H burning Isochrones (0.6-2.0) Gyr

Ref: Cassisi S., Castellani M. & Castellani V., A&A, 317, 108

1997.2

Old metal rich  populations

Z=0.02, Y=0.289
 

H- & He-burning tracks (0.5-3.0)Mo

Horizontal Branch tracks RGB progenitors: (0.8 to 2.1)Mo

Isochrones (1 to 18)Gyr

Z=0.01, Y=0.255
 

H- & He-burning tracks (0.6 to 3.0)Mo

Horizontal Branch tracks RGB progenitors: (1.0-2.0)Mo

Isochrones  (1 to 18)Gyr

Ref: Bono G., Caputo F., Cassisi S., Castellani V., Marconi M. , ApJ, 479, 279

1997.3

Old  super metal-rich populations
 

Z=0.04  Y=0.34	H- & He-burning tracks (0.6 to 3.0)Mo	Horizontal Branch tracks RGB progenitors: 1.0. 1.8. 2.0 Mo	Isochrones  (1 to 18)Gyr
Z=0.04 Y=0.37	H- & He-burning tracks (0.6 to 3.0)Mo	Horizontal Branch tracks RGB progenitors: 1.0. 1.5, 1.8  Mo

Ref: Bono G., Caputo F., Cassisi S., Castellani V., Marconi M., ApJ, 489, 822

1997.4

Evolutionary models for Very Low-Mass  MS STARS
 

Age = 10 Gyr	VLM models Z=0.0001, 0.0003, 0.0006, 0.001 (0.093 to 0.6)Mo
Age= 20 Gyr	VLM models Z=0.0001, 0.0003, 0.0006, 0.001 (0.093 to 0.6)Mo

Note 1: Outer boundary conditions fixed by adopting the Eddington's approximation.

Ref: Alexander D.R., Brocato E., Cassisi S., Castellani V., Ciacio F. & Degl'Innocenti S., A&A, 317, 90

1998.1

Evolutionary models for Very Low-Mass MS stars
 

VLM models Z=0.0002 Y=0.23 Z=0.002   Y=0.23 Z=0.02     Y=0.27 (0.95 to 0.7)Mo

 Note 1: Outer boundary conditions fixed by adopting the model atmospheres by Brett (1995)

 Ref: Brocato E., Cassisi S. & Castellani V., MNRAS, 295, 711

1998.2

Evolutionary models for H-burning, low-mass, metal-poor stars.
 
 

Z=0.0002 - Y=0.23 - standard - ml=1.6	H-Burning models (0.7-0.9)Mo	Horizontal branch models	isochrones (8-18)Gyr
Z=0.0002 - Y=0.23 - diffusion - ml=1.6	H-Burning models (0.6-1.0)Mo	Horizontal branch models	isochrones (8-18)Gyr
Z=0.001 - Y=0.23 - standard - ml=1.6	H-Burning models (0.6-1.0)Mo	Horizontal branch models	isochrones (8-20)Gyr
Z=0.001 - Y=0.23 - diffusion - ml=1.6	H-Burning models (0.6-1.0)Mo	Horizontal branch models	isochrones (8-18)Gyr
Z=0.006 - Y=0.23 - diffusion - ml=1.6	H-Burning models (0.65-1.0)Mo	Horizontal branch models	isochrones (9.5-20)Gyr
Z=0.006 - Y=0.23 - standard - ml=1.8	H-Burning models (0.65-1.0)Mo	Horizontal branch models	isochrones (9.5-20)Gyr
Z=0.006 - Y=0.23 - diffusion - ml=1.8	H-Burning models (0.65-1.0)Mo	Horizontal branch models	isochrones (9.5-18)Gyr

Note 1: Standard = no diffusion; ml = mixing length
Note 2: Implemented in 1999.1

Ref: Cassisi S., Castellani V., Degl'Innocenti S. & Weiss A., A&ASS, 129, 267

1999.1

Evolutionary models for H-burning, low-mass, metal-poor stars
 
 

Z=0.0006 - Y=0.23 - standard - ml=1.6	H-Burning models (0.6-1.0)Mo	Horizontal branch models	isochrones (8-18)Gyr
Z=0.0006 - Y=0.23 - diffusion - ml=1.6	H-Burning models (0.6-1.0)Mo	Horizontal branch models	isochrones (8-18)Gyr
Z=0.001 - Y=0.21 - diffusion - ml=1.6	H-Burning models (0.6-1.0)Mo		isochrones (8-17)Gyr
Z=0.001 - Y=0.25 - diffusion - ml=1.6	H-Burning models (0.6-1.0)Mo		isochrones (8-17)Gyr

 Ref: Cassisi S., Castellani V., Degl'Innocenti S., Salaris M. & Weiss A., A&ASS, 134, 103

1999.2

Evolutionary models for H- and He-burning, low- and intermediate-mass stars
 
 

Z=0.001 - Y=0.23 - diffusion ml=1.9	H-burning models (0.7 - 2.0)Mo	He burning models  (1.0 - 2.0) Mo	isochrones (1 - 6) Gyr
Z=0.004 - Y=0.238 - diffusion ml=1.9	H-burning models  (0.65 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1-6) Gyr
Z=0.004 - Y=0.270 - diffusion ml=1.9	H- & He-burning models (0.7 - 8.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (0.05 - 5.5) Gyr
Z=0.007 - Y=0.244 - diffusion ml=1.9	H-burning models  (0.7 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1 - 7) Gyr
Z=0.007 - Y=0.270 - diffusion ml=1.9	H-burning models  (0.6 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1 - 9.5) Gyr
Z=0.007 - Y=0.270 - standard ml=1.6	H-burning models (0.6 - 2.0) Mo	He burning models  (1.0 - 2.0) Mo	isochrones (1 - 6) Gyr
Z=0.010 - Y=0.270 - diffusion ml=1.9	H-burning models  (0.65 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1 - 11) Gyr
Z=0.010 - Y=0.270 - standard ml=1.6	H-burning models  (0.6 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1 - 10) Gyr
Z=0.015 - Y=0.230 - diffusion ml=1.9	H-burning models (0.7 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1.5 - 11) Gyr
Z=0.015 - Y=0.270 - diffusion ml=1.9	H-burning model (0.65 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1 - 10) Gyr
Z=0.015 - Y=0.270 - standard ml=1.6	H-burning models (0.65 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1.5 - 11) Gyr
Z=0.015 - Y=0.270 - standard ml=2.2			isochrones (0.3 - 12) Gyr
Z=0.015 - Y=0.270 - standard ml=1.0			isochrones (0.3 - 12) Gyr
Z=0.020 - Y=0.230 - diffusion ml=1.9	H-burning models (0.7 - 2.7) Mo	He burning models (1.0 - 2.7) Mo	isochrones (0.8 - 12) Gyr
Z=0.020 - Y=0.270 - diffusion ml=1.9	H-burning models (0.6 - 2.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (1.0 - 10) Gyr
Z=0.020 - Y=0.270 - diffusion ml=1.6	H- & He-burning models (0.6-9.0) Mo	He burning models (1.0 - 2.0) Mo	isochrones (0.1 - 10) Gyr

  Ref: Castellani V., Degl'Innocenti S. & Marconi M., MNRAS, 303, 265
 

2000.1

Galactic globular clusters as a test for Very Low-Mass stellar models
 

VLM models Z=0.0002   Y=0.23 Z=0.0006   Y=0.23 Z=0.001     Y=0.23 Z=0.002     Y=0.23 (0.09 to 0.8)Mo

Note 1: Outer boundary conditions fixed by adopting the model atmospheres by Allard & Hauschildt (1997, 1999)

Ref: Cassisi S., Castellani V., Ciarcelluti P., Piotto G. & Zoccali M., MNRAS, 315, 679
 

 2000.2

Intermediate-mass star models with different helium and metal contents
 
 
 

Z=0.004

H- and He-burning models Y=0.23

H- and He-burning models Y=0.27

Z=0.01

H- and He-burning models Y=0.23

H- and He-burning models Y=0.255

H- and He-burning models Y=0.27

Z=0.02

H- and He-burning models Y=0.27

H- and He-burning models Y=0.289

Z=0.04

H- and He-burning models Y=0.29

H- and He-burning models Y=0.34

H- and He-burning models Y=0.37

 

  Ref: Bono G., Caputo F., Cassisi S., Marconi M., Piersanti L. & Tornambe' A.,  ApJ, 543, 955
 
 

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