Young stars in the Galactic Centre: a potential intermediate-mass star origin
(2006) In Monthly Notices of the Royal Astronomical Society 372(1). p.31-44- Abstract
- There has been recent speculation that the cores of intermediate-mass stars stripped of their envelopes by tidal interaction with the supermassive black hole in the Galactic Centre could form a population observationally similar to the so-called Sgr A* cluster or 'S' stars, which have close eccentric orbits around the hole. We model the evolution of such stars, and show that the more luminous end of the population may indeed appear similar to young B stars within the observational limits of the Galactic Centre region. Whether some or all of these cluster stars can be accounted for in this manner depends strongly on the assumed initial mass function (IMF) of the loss cone stars and the scattering rate. If most of the observed stars are in... (More)
- There has been recent speculation that the cores of intermediate-mass stars stripped of their envelopes by tidal interaction with the supermassive black hole in the Galactic Centre could form a population observationally similar to the so-called Sgr A* cluster or 'S' stars, which have close eccentric orbits around the hole. We model the evolution of such stars, and show that the more luminous end of the population may indeed appear similar to young B stars within the observational limits of the Galactic Centre region. Whether some or all of these cluster stars can be accounted for in this manner depends strongly on the assumed initial mass function (IMF) of the loss cone stars and the scattering rate. If most of the observed stars are in fact scattered from the Galactic Centre inner cusp region itself then the population of similar to 20 to current observational limits may be reproduced. However, this only works if the local relaxation time is small and relies on the cusp stars themselves being young, i.e. it is dependent on some star formation being possible in the central few parsecs. Conversely, we obtain a possible constraint on the tidal stripping rate of 'normal' IMF stars if there are not to be red stars visible in the Sgr A* cluster. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/392629
- author
- Dray, L. M. ; King, A. R. and Davies, Melvyn B LU
- organization
- publishing date
- 2006
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Galaxy : centre, stars : early-type, stars : kinematics, Galaxy :, stellar content
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 372
- issue
- 1
- pages
- 31 - 44
- publisher
- Oxford University Press
- external identifiers
-
- wos:000240823800003
- scopus:33749181551
- ISSN
- 1365-2966
- DOI
- 10.1111/j.1365-2966.2006.10841.x
- language
- English
- LU publication?
- yes
- id
- d136e024-dc27-4e8b-b5e1-ff39da0385a6 (old id 392629)
- date added to LUP
- 2016-04-01 12:14:25
- date last changed
- 2024-01-08 13:21:42
@article{d136e024-dc27-4e8b-b5e1-ff39da0385a6,
abstract = {{There has been recent speculation that the cores of intermediate-mass stars stripped of their envelopes by tidal interaction with the supermassive black hole in the Galactic Centre could form a population observationally similar to the so-called Sgr A* cluster or 'S' stars, which have close eccentric orbits around the hole. We model the evolution of such stars, and show that the more luminous end of the population may indeed appear similar to young B stars within the observational limits of the Galactic Centre region. Whether some or all of these cluster stars can be accounted for in this manner depends strongly on the assumed initial mass function (IMF) of the loss cone stars and the scattering rate. If most of the observed stars are in fact scattered from the Galactic Centre inner cusp region itself then the population of similar to 20 to current observational limits may be reproduced. However, this only works if the local relaxation time is small and relies on the cusp stars themselves being young, i.e. it is dependent on some star formation being possible in the central few parsecs. Conversely, we obtain a possible constraint on the tidal stripping rate of 'normal' IMF stars if there are not to be red stars visible in the Sgr A* cluster.}},
author = {{Dray, L. M. and King, A. R. and Davies, Melvyn B}},
issn = {{1365-2966}},
keywords = {{Galaxy : centre; stars : early-type; stars : kinematics; Galaxy :; stellar content}},
language = {{eng}},
number = {{1}},
pages = {{31--44}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{Young stars in the Galactic Centre: a potential intermediate-mass star origin}},
url = {{http://dx.doi.org/10.1111/j.1365-2966.2006.10841.x}},
doi = {{10.1111/j.1365-2966.2006.10841.x}},
volume = {{372}},
year = {{2006}},
}