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Star Formation Close to Sgr A* and Beyond the Nuclear Cluster

Published online by Cambridge University Press:  23 June 2017

Farhad Yusef-Zadeh  and
Mark Wardle
Farhad Yusef-Zadeh
Affiliation:
CIERA, Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Rd, Evanston, IL 60208, US email: [email protected]
Mark Wardle
Affiliation:
2Department of Physics and Astronomy and Research Center for Astronomy, Astrophysics & Astrophotonics, Macquarie University, Sydney NSW 2109, Australia email: [email protected]
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Abstract

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Two modes of star formation are involved to explain the origin of young stars near Sgr A*. One is a disk-based mode, which explains the disk of stars orbiting Sgr A*. The other is the standard cloud-based mode observed in the Galactic disk. We discuss each of these modes of star formation and apply these ideas to the inner few parsecs of Sgr A*. In particular, we focus on the latter mode in more detail. We also discuss how the tidal force exerted by the nuclear cluster makes the Roche density approaching zero and contributes to the collapse of molecular clouds located tens of parsecs away from Sgr A*.

Keywords

Galaxy: nucleusstars: formationISM: clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S324: New Frontiers in Black Hole Astrophysics , September 2016 , pp. 111 - 114
Copyright
Copyright © International Astronomical Union 2017 

References

Chen, X., Amaro-Seoane, P., & Cuadra, J. 2016, ApJ, 819, 138 CrossRefGoogle Scholar
Geballe, T. R., Najarro, F., Rigaut, F., & Roy, J.-R. 2006, ApJ, 652, 370 CrossRefGoogle Scholar
Jog, C. J. 2013, MNRAS, 434, L56 Google Scholar
Lu, J. R., Ghez, A. M., Hornstein, S. D., et al. 2009, ApJ, 690, 1463 Google Scholar
Paumard, T., Genzel, R., Martins, F., et al. 2006, ApJ, 643, 1011 CrossRefGoogle Scholar
Sanchez-Bermudez, J., Alberdi, A., Schödel, R., et al. 2014, A&AP, 572, L1 Google Scholar
Stolte, A., Brandner, W., Grebel, E. K., Lenzen, R., & Lagrange, A.-M. 2005, ApJ, 628, L113 CrossRefGoogle Scholar
Tsuboi, M., Kitamura, Y., Miyoshi, M., et al. 2016, PASJ, 68, L7 Google Scholar
Wardle, M. & Yusef-Zadeh, F. 2008, ApJ, 683, L37 CrossRefGoogle Scholar
Wardle, M. & Yusef-Zadeh, F. 2014, ApJ, 787, L14 CrossRefGoogle Scholar
Yusef-Zadeh, F., Royster, M., Wardle, M., et al. 2013, ApJ, 767, L32 Google Scholar
Yusef-Zadeh, F., Roberts, D. A., & Wardle, M., et al. 2015b, ApJ, 801, L26 CrossRefGoogle Scholar
Yusef-Zadeh, F., Wardle, M., Sewilo, M., et al. 2015a, ApJ, 808, 97 Google Scholar