Bar - 版本历史

2025年12月29日 (一) 10:34 Shen

2025-12-29T10:34:21Z

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	* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.		* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.
	* hypothesis： that fast bars are formed by global instabilities in isolated galaxies, while slow bars are triggered by tidal interactions in dense environments arXiv:2511.02054		* hypothesis： that fast bars are formed by global instabilities in isolated galaxies, while slow bars are triggered by tidal interactions in dense environments arXiv:2511.02054

			==形成机制==
			* Can A Kinematically Hot and Thick Disk Form A Bar? : Role of Highly Spinning Dark Matter Halos arXiv:2512.21632
			:*高红移星系，动力学上更热，看到了棒结构，可能与旋转的晕有关。

2025年11月5日 (三) 10:39 Shen

2025-11-05T10:39:38Z

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	* CR is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed.		* CR is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed.
	* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.		* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.
			* hypothesis： that fast bars are formed by global instabilities in isolated galaxies, while slow bars are triggered by tidal interactions in dense environments arXiv:2511.02054

Shen：/* pattern speed */

2024-09-23T14:19:23Z

pattern speed

←上一版本		2024年9月23日 (一) 14:19的版本
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	==pattern speed==		==pattern speed==
	* the rotational frequency of the bar.		defined as the rotational frequency of the bar.
	* ~~physical upper limit: bar~~ cannot extend beyond the corotation resonance (CR) radius		* Bar cannot extend beyond the corotation resonance (CR) radius of the galaxy.
	of ~~the galaxy, which~~ is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed.		* CR is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed.
	* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) ~~can�not~~ support a bar structure.		* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) cannot support a bar structure.

Shen：/* strength */

2024-09-23T14:17:56Z

strength

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	==strength==		==strength==
	The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential		The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002).
		⚫	* measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block , 2001; Laurikainen et al. , 2007; Salo et al. , 2010)
	in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002).
		⚫	* bar ellipticity Martinet & Friedli (1997); Aguerri (1999); Whyte et al. (2002); Marinova & Jogee (2007); Aguerri et al. (2009)
⚫	* measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block ,
		⚫	* Fourier decomposition of the galaxy light Ohta et al. (1990); Marquez et al. (1996); Aguerri et al. (2000); Athanassoula & Misiriotis (2002); Laurikainen et al. (2005).
	2001; Laurikainen et al. , 2007; Salo et al. , 2010)
⚫	* bar ellipticity Martinet & Friedli (1997); Aguerri (1999); Whyte et al.
	(2002); Marinova & Jogee (2007); Aguerri et al. (2009)
	* Fourier decomposition of the galaxy light Ohta et al.
⚫	(1990); Marquez et al. (1996); Aguerri et al. (2000); Athanassoula & Misiriotis (2002); Laurikainen et al. (2005).

	==pattern speed==		==pattern speed==

Shen：创建页面，内容为“描述棒星系的三个参数，长度，强度，和pattern speed [https://arxiv.org/pdf/1501.05498] ==strength== The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002). measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block , 2001; Laurikainen et al. , 2007; Salo et al. , 2010) * bar ellipticity Martin…”

2024-09-23T14:17:07Z

创建页面，内容为“*描述棒星系的三个参数，长度，强度，和pattern speed [https://arxiv.org/pdf/1501.05498] ==strength== The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002). * measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block , 2001; Laurikainen et al. , 2007; Salo et al. , 2010) * bar ellipticity Martin…”

新页面

*描述棒星系的三个参数，长度，强度，和pattern speed [https://arxiv.org/pdf/1501.05498]

==strength==
The bar strength is a parameter that measures the non-axisymmetric forces produced by the bar potential
in the disc of galaxies (see, e.g., Laurikainen & Salo, 2002).
* measure the torques of the bar (e.g., Combes & Sanders , 1981; Quillen et al. , 1994; Buta & Block ,
2001; Laurikainen et al. , 2007; Salo et al. , 2010)
* bar ellipticity Martinet & Friedli (1997); Aguerri (1999); Whyte et al.
(2002); Marinova & Jogee (2007); Aguerri et al. (2009)
* Fourier decomposition of the galaxy light Ohta et al.
(1990); Marquez et al. (1996); Aguerri et al. (2000); Athanassoula & Misiriotis (2002); Laurikainen et al. (2005).

==pattern speed==
* the rotational frequency of the bar.
* physical upper limit: bar cannot extend beyond the corotation resonance (CR) radius
of the galaxy, which is the region of the galaxy where the angular speed of the stars of the disc in circular motions equals the bar pattern speed.
* This limit is imposed by the stability of the main family of orbits forming the bar (the so-called x1 family; Contopoulos 1980) which are only stable within R(CR). Orbits in the outer region of the disc (R > RCR) can�not support a bar structure.

Bar - 版本历史

2025年12月29日 (一) 10:34 Shen

2025年11月5日 (三) 10:39 Shen

Shen：​/* pattern speed */

Shen：​/* strength */

Shen：/* pattern speed */

Shen：/* strength */