2016A&A...588A..42S


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.18CEST10:58:52

2016A&A...588A..42S - Astronomy and Astrophysics, volume 588A, 42-42 (2016/4-1)

Spin-up of massive classical bulges during secular evolution.

SAHA K., GERHARD O. and MARTINEZ-VALPUESTA I.

Abstract (from CDS):

Context. Classical bulges in spiral galaxies are known to rotate, but the origin of this observed rotational motion is not well understood. It has been shown recently that a low-mass classical bulge (ClB) in a barred galaxy can acquire rotation by absorbing a significant fraction of the angular momentum emitted by the bar.
Aims. Our aim here is to investigate whether bars can also spin up more massive ClBs during the secular evolution of the bar, and to study the kinematics and dynamics of these ClBs.
Methods. We use a set of self-consistent N-body simulations to study the interaction of ClBs with a bar that forms self-consistently in the disk. We use orbital spectral analysis to investigate the angular momentum gain by the classical bulge stars.
Results. We show that the ClBs gain on average 2-6% of the disk's initial angular momentum within the bar region. Most of this angular momentum gain occurs via low-order resonances, particularly 5:2 resonant orbits. A density wake forms in the ClB which corotates and aligns with the bar at the end of the evolution. The spin-up process creates a characteristic linear rotation profile and mild tangential anisotropy in the ClB. The induced rotation is small in the centre, but is significant beyond ∼2 bulge half mass radii, where it leads to mass-weighted V/σ∼0.2, and reaches a local Vmaxin∼0.5 at around the scale of the bar. The resulting V/σ is tightly correlated with the ratio of the bulge size to the bar size. In all models, a box/peanut bulge forms suggesting that composite bulges may be common.
Conclusions. Bar-bulge resonant interaction in barred galaxies can provide some spin-up of massive ClBs, but the process appears to be less efficient than for low-mass ClBs. Further angular momentum transfer due to nuclear bars or gas inflow would be required to explain the observed rotation if it is not primordial.

Abstract Copyright: © ESO, 2016

Journal keyword(s): galaxies: bulges - galaxies: structure - galaxies: kinematics and dynamics - galaxies: spiral - galaxies: evolution

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 1023 IG 02 40 24.012 +39 03 47.70 10.91 10.35 9.35 7.83   ~ 604 2
2 NGC 2775 G 09 10 20.112 +07 02 16.53   11.417 10.481 9.920 8.994 ~ 320 0
3 NGC 2841 LIN 09 22 02.655 +50 58 35.32 10.43 10.09 9.22     ~ 992 1
4 NGC 2859 G 09 24 18.549 +34 30 48.16   11.8       ~ 237 0
5 NGC 2880 GiG 09 29 34.618 +62 29 26.23   12.6       ~ 137 0
6 M 81 Sy2 09 55 33.17306143 +69 03 55.0609270   7.89 6.94     ~ 3984 5
7 NGC 3245 GiP 10 27 18.3853542210 +28 30 26.626222848   11.6       ~ 314 0
8 NGC 3521 LSB 11 05 48.5676206040 -00 02 09.228156576 10.06 9.83 9.02 10.1 9.6 ~ 703 2
9 NGC 3898 LIN 11 49 15.370 +56 05 03.66   11.7       ~ 268 1
10 M 109 GiG 11 57 35.984 +53 22 28.27   10.94   9.57   ~ 417 0
11 NGC 4260 GiP 12 19 22.247 +06 05 55.69   13.1       ~ 147 0
12 NGC 4698 Sy2 12 48 22.9112380605 +08 29 14.648866444   13.24 12.27     ~ 444 0
13 NGC 4772 LIN 12 53 29.1636622578 +02 10 06.133021648 12.29 11.96 11.04     ~ 221 1

    Equat.    Gal    SGal    Ecl

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2020.09.18-10:58:52

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