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Revista mexicana de astronomía y astrofísica

Print version ISSN 0185-1101

Rev. mex. astron. astrofis vol.46 n.1 Ciudad de México Apr. 2010

 

Age Estimation And Masss Functions of TTauri Stars in The Taurus Auriga Molecular Cloud

 

I. Küçük1 and I. Akkaya1

 

1 Department of Astronomy and Space Sciences, Faculty of Arts and Sciences, Erciyes University, Talas Yolu, 38039, Kayseri, Turkey. (kucuk@erciyes.edu.tr, akkaya@erciyes.edu.tr).

 

Received 2009 July 10
Accepted 2009 December 14

 

RESUMEN

En este trabajo se han calculado las funciones de masas en la actualidad (PDMF) de las estrellas T–Tauri (TTS) que están en la fase evolutiva de pre–secuencia principal (PMS) en el complejo de nubes moleculares de Taurus–Auriga. Con este fin, mediante la aplicación de nuestro código modificado de evolución estelar se utilizan modelos estelares en el intervalo de masa de 0.1 – 2.5 para determinar la masa y la masa de edad de las TTS. La función de la masa obtenida se compara con la función de masa de Miller & Scalo (1979). La edad encontrada para las TTS es de alrededor de 1 – 3 × 106 años y la función de masa es de aproximadamente 0.6440.348. De estos resultados, hemos calculado la tasa de formación estelar como de alrededor de 1.3 × 10–7 año–1 en esta región.

 

ABSTRACT

In this work the present day mass functions (PDMF) of T–Tauri Stars (TTS) which are in the pre–main sequence (PMS) evolutionary phase of their evolution in the Taurus–Auriga Molecular Cloud Complex have been calculated. For this purpose, by applying our modified stellar evolutionary code, stellar models in the mass range 0.1 – 2.5 are used to determine the mass and age mass of TTS. The obtained mass function is compared with the mass function of Miller & Scalo (1979). The age found for TTS is around 1 – 3 × 106 yr and the mass function is about 0.6440.348. From these results, we have calculated the stellar birthrate as about 1.3 × 10–7 yr –1 in this region.

Key Words: open clusters and associations: general — stars: evolution — stars: fundamental parameters — stars: pre–main sequence.

 

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ACKNOWLEDGMENTS

This work was supported by the Section of Scientic Research Projects (EUBAP) of the Erciyes University, Project number: FBT–05–36.

 

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