Orbital Support and Evolution of Flat Profiles of Bars (Shoulders)
Abstract Many barred galaxies exhibit upturns (shoulders) in their bar-major-axis density profile. Simulation studies have suggested that shoulders are supported by looped x 1 orbits, occur in growing bars, and can appear after bar buckling. We investigate the orbital support and evolution of should...
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Published in | The Astrophysical journal Vol. 955; no. 1; pp. 38 - 62 |
---|---|
Main Authors | , , , , , , |
Format | Journal Article |
Language | English |
Published |
Philadelphia
The American Astronomical Society
01.09.2023
IOP Publishing |
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Abstract | Abstract
Many barred galaxies exhibit upturns (shoulders) in their bar-major-axis density profile. Simulation studies have suggested that shoulders are supported by looped
x
1
orbits, occur in growing bars, and can appear after bar buckling. We investigate the orbital support and evolution of shoulders via frequency analyses of orbits in simulations. We confirm that looped orbits are shoulder-supporting, and can remain so, to a lesser extent, after being vertically thickened. We show that looped orbits appear at the resonance ( Ω
φ
− Ω
P
)/Ω
R
= 1/2 (analogous to the classical inner Lindblad resonance, and here called ILR) with vertical-to-radial frequency ratios 1 ≲ Ω
z
/Ω
R
≲ 3/2 (vertically
warm
orbits).
Cool
orbits at the ILR (those with Ω
z
/Ω
R
> 3/2) are vertically thin and have no loops, contributing negligibly to shoulders. As bars slow and thicken, either secularly or by buckling, they populate warm orbits at the ILR. Further thickening carries these orbits toward crossing the vertical ILR [vILR, ( Ω
φ
− Ω
P
)/Ω
z
= 1/2], where they convert in-plane motion to vertical motion, become chaotic, kinematically hotter, and less shoulder-supporting. Hence, persistent shoulders require bars to trap new stars, consistent with the need for a growing bar. Since buckling speeds up trapping on warm orbits at the ILR, it can be followed by shoulder formation, as seen in simulations. This sequence supports the recent observational finding that shoulders likely precede the emergence of BP-bulges. The python module for the frequency analysis,
naif
, is made available. |
---|---|
AbstractList | Abstract
Many barred galaxies exhibit upturns (shoulders) in their bar-major-axis density profile. Simulation studies have suggested that shoulders are supported by looped
x
1
orbits, occur in growing bars, and can appear after bar buckling. We investigate the orbital support and evolution of shoulders via frequency analyses of orbits in simulations. We confirm that looped orbits are shoulder-supporting, and can remain so, to a lesser extent, after being vertically thickened. We show that looped orbits appear at the resonance ( Ω
φ
− Ω
P
)/Ω
R
= 1/2 (analogous to the classical inner Lindblad resonance, and here called ILR) with vertical-to-radial frequency ratios 1 ≲ Ω
z
/Ω
R
≲ 3/2 (vertically
warm
orbits).
Cool
orbits at the ILR (those with Ω
z
/Ω
R
> 3/2) are vertically thin and have no loops, contributing negligibly to shoulders. As bars slow and thicken, either secularly or by buckling, they populate warm orbits at the ILR. Further thickening carries these orbits toward crossing the vertical ILR [vILR, ( Ω
φ
− Ω
P
)/Ω
z
= 1/2], where they convert in-plane motion to vertical motion, become chaotic, kinematically hotter, and less shoulder-supporting. Hence, persistent shoulders require bars to trap new stars, consistent with the need for a growing bar. Since buckling speeds up trapping on warm orbits at the ILR, it can be followed by shoulder formation, as seen in simulations. This sequence supports the recent observational finding that shoulders likely precede the emergence of BP-bulges. The python module for the frequency analysis,
naif
, is made available. Many barred galaxies exhibit upturns (shoulders) in their bar-major-axis density profile. Simulation studies have suggested that shoulders are supported by looped x _1 orbits, occur in growing bars, and can appear after bar buckling. We investigate the orbital support and evolution of shoulders via frequency analyses of orbits in simulations. We confirm that looped orbits are shoulder-supporting, and can remain so, to a lesser extent, after being vertically thickened. We show that looped orbits appear at the resonance ( Ω _φ − Ω _P )/Ω _R = 1/2 (analogous to the classical inner Lindblad resonance, and here called ILR) with vertical-to-radial frequency ratios 1 ≲ Ω _z /Ω _R ≲ 3/2 (vertically warm orbits). Cool orbits at the ILR (those with Ω _z /Ω _R > 3/2) are vertically thin and have no loops, contributing negligibly to shoulders. As bars slow and thicken, either secularly or by buckling, they populate warm orbits at the ILR. Further thickening carries these orbits toward crossing the vertical ILR [vILR, ( Ω _φ − Ω _P )/Ω _z = 1/2], where they convert in-plane motion to vertical motion, become chaotic, kinematically hotter, and less shoulder-supporting. Hence, persistent shoulders require bars to trap new stars, consistent with the need for a growing bar. Since buckling speeds up trapping on warm orbits at the ILR, it can be followed by shoulder formation, as seen in simulations. This sequence supports the recent observational finding that shoulders likely precede the emergence of BP-bulges. The python module for the frequency analysis, naif , is made available. Many barred galaxies exhibit upturns (shoulders) in their bar-major-axis density profile. Simulation studies have suggested that shoulders are supported by looped x1 orbits, occur in growing bars, and can appear after bar buckling. We investigate the orbital support and evolution of shoulders via frequency analyses of orbits in simulations. We confirm that looped orbits are shoulder-supporting, and can remain so, to a lesser extent, after being vertically thickened. We show that looped orbits appear at the resonance ( Ωφ − ΩP)/ΩR = 1/2 (analogous to the classical inner Lindblad resonance, and here called ILR) with vertical-to-radial frequency ratios 1 ≲ Ωz/ΩR ≲ 3/2 (vertically warm orbits). Cool orbits at the ILR (those with Ωz/ΩR > 3/2) are vertically thin and have no loops, contributing negligibly to shoulders. As bars slow and thicken, either secularly or by buckling, they populate warm orbits at the ILR. Further thickening carries these orbits toward crossing the vertical ILR [vILR, ( Ωφ − ΩP)/Ωz = 1/2], where they convert in-plane motion to vertical motion, become chaotic, kinematically hotter, and less shoulder-supporting. Hence, persistent shoulders require bars to trap new stars, consistent with the need for a growing bar. Since buckling speeds up trapping on warm orbits at the ILR, it can be followed by shoulder formation, as seen in simulations. This sequence supports the recent observational finding that shoulders likely precede the emergence of BP-bulges. The python module for the frequency analysis, naif, is made available. |
Author | Valluri, Monica Debattista, Victor P. Anderson, Stuart Robert Erwin, Peter Daniel, Kathryne J. Deg, Nathan Beraldo e Silva, Leandro |
Author_xml | – sequence: 1 givenname: Leandro orcidid: 0000-0002-0740-1507 surname: Beraldo e Silva fullname: Beraldo e Silva, Leandro organization: University of Central Lancashire Jeremiah Horrocks Institute, Preston PR1 2HE, UK – sequence: 2 givenname: Victor P. orcidid: 0000-0001-7902-0116 surname: Debattista fullname: Debattista, Victor P. organization: University of Central Lancashire Jeremiah Horrocks Institute, Preston PR1 2HE, UK – sequence: 3 givenname: Stuart Robert orcidid: 0000-0002-6379-5053 surname: Anderson fullname: Anderson, Stuart Robert organization: University of Central Lancashire Jeremiah Horrocks Institute, Preston PR1 2HE, UK – sequence: 4 givenname: Monica orcidid: 0000-0002-6257-2341 surname: Valluri fullname: Valluri, Monica organization: University of Michigan Department of Astronomy, 1085 S. University Avenue, Ann Arbor, MI 48109 ; USA – sequence: 5 givenname: Peter orcidid: 0000-0003-4588-9555 surname: Erwin fullname: Erwin, Peter organization: Max Planck Institut für Extraterrestrische Physik , Giessenbachstrasse, D-85748 Garching, Germany – sequence: 6 givenname: Kathryne J. orcidid: 0000-0003-2594-8052 surname: Daniel fullname: Daniel, Kathryne J. organization: Flatiron Institute Center for Computational Astrophysics, New York, NY 10010, USA – sequence: 7 givenname: Nathan orcidid: 0000-0003-3523-7633 surname: Deg fullname: Deg, Nathan organization: Queen’s University Department of Physics, Engineering Physics, and Astronomy, Kingston, ON, K7L 3N6, Canada |
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CitedBy_id | crossref_primary_10_3847_1538_4357_ace962 crossref_primary_10_1093_mnras_stad3907 crossref_primary_10_1016_j_newast_2024_102247 crossref_primary_10_3847_2041_8213_ad2465 |
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Many barred galaxies exhibit upturns (shoulders) in their bar-major-axis density profile. Simulation studies have suggested that shoulders are... Many barred galaxies exhibit upturns (shoulders) in their bar-major-axis density profile. Simulation studies have suggested that shoulders are supported by... |
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StartPage | 38 |
SubjectTerms | Astrophysics Barred galaxies Buckling Evolution Frequency analysis Galactic bar Galaxy bars Galaxy dynamics Lindblad resonance N-body simulations Orbital resonances (celestial mechanics) Orbits Resonance Shoulder Simulation Vertical motion |
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Title | Orbital Support and Evolution of Flat Profiles of Bars (Shoulders) |
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