# User:Tohline/SSC/Structure/LimitingMasses

(Difference between revisions)
 Revision as of 09:55, 25 October 2014 (view source)Tohline (Talk | contribs) (→Relationship Between the Bonnor-Ebert and Schönberg-Chandrasekhar Critical Masses: Insert embedded polytrope virial-equilibrium figure)← Older edit Current revision as of 10:22, 19 November 2020 (view source)Tohline (Talk | contribs) (→Related Discussions) (5 intermediate revisions not shown) Line 2: Line 2: =Mass Upper Limits= =Mass Upper Limits= {{LSU_HBook_header}} {{LSU_HBook_header}} - Spherically symmetric, self-gravitating, equilibrium configurations can be constructed from gases exhibiting a wide variety of degrees of compressibility.  When examining how the internal structure of such configurations varies with compressibility, or when examining the relative stability of such structures, it can be instructive to construct models using a polytropic equation of state because the degree of compressibility can be adjusted by simply changing the value of the polytropic index, {{User:Tohline/Math/MP_PolytropicIndex}}, across the range, $0 \le n \le \infty$.  (Alternatively, one can vary the effective adiabatic exponent of the gas, $\gamma_g = 1 + 1/n$.)  In particular, $n = 0$ ($\gamma_g = \infty$) represents a ''hard'' equation of state and describes an incompressible configuration, while $n = \infty$ ($\gamma_g = 1$) represents an isothermal and extremely ''soft'' equation of state. + Spherically symmetric, self-gravitating, equilibrium configurations can be constructed from gases exhibiting a wide variety of degrees of compressibility.  When examining how the internal structure of such configurations varies with compressibility, or when examining the relative stability of such structures, it can be instructive to construct models using a polytropic equation of state because the degree of compressibility can be adjusted by simply changing the value of the polytropic index, {{User:Tohline/Math/MP_PolytropicIndex}}, across the range, $~0 \le n \le \infty$.  (Alternatively, one can vary the effective adiabatic exponent of the gas, $~\gamma_g = 1 + 1/n$.)  In particular, $~n = 0 ~~ (\gamma_g = \infty)$ represents a ''hard'' equation of state and describes an incompressible configuration, while $~n = \infty ~~(\gamma_g = 1)$ represents an isothermal and extremely ''soft'' equation of state. ==Isolated Polytropes== ==Isolated Polytropes== [[User:Tohline/SSC/Structure/Polytropes#Polytropic_Spheres|Isolated polytropic spheres]] exhibit three attributes that are especially key in the context of our present discussion: [[User:Tohline/SSC/Structure/Polytropes#Polytropic_Spheres|Isolated polytropic spheres]] exhibit three attributes that are especially key in the context of our present discussion:
-
1. The equilibrium structure is dynamically stable if $n < 3$. +
2. The equilibrium structure is dynamically stable if $~n < 3$. -
3. The equilibrium structure has a finite radius if $n < 5$. +
4. The equilibrium structure has a finite radius if $~n < 5$. -
5. The equilibrium structure can be described in terms of closed-form analytic expressions for [[User:Tohline/SSC/Structure/Polytropes#n_.3D_0_Polytrope|$n = 0$]], +
6. The equilibrium structure can be described in terms of closed-form analytic expressions for [[User:Tohline/SSC/Structure/Polytropes#n_.3D_0_Polytrope|$~n = 0$]], - [[User:Tohline/SSC/Structure/Polytropes#n_.3D_1_Polytrope|$n = 1$]], and + [[User:Tohline/SSC/Structure/Polytropes#n_.3D_1_Polytrope|$~n = 1$]], and - [[User:Tohline/SSC/Structure/Polytropes#n_.3D_5_Polytrope|$n = 5$]]. + [[User:Tohline/SSC/Structure/Polytropes#n_.3D_5_Polytrope|$~n = 5$]].
==Isothermal Spheres== ==Isothermal Spheres== - Isothermal spheres (polytropes with index $n=\infty$) are discussed in a wide variety of astrophysical contexts because it is not uncommon for physical conditions to conspire to create an extended volume throughout which a configuration exhibits uniform temperature.  But [[User:Tohline/SSC/Structure/IsothermalSphere#Isothermal_Sphere|mathematical models of isothermal spheres]] are relatively cumbersome to analyze because they extend to infinity, they are dynamically unstable, and they are not describable in terms of analytic functions.  In such astrophysical contexts, we have sometimes found it advantageous to employ an $n=5$ polytrope instead of an isothermal sphere.  An [[User:Tohline/SSC/Structure/Polytropes#n_.3D_5_Polytrope|isolated $n=5$ polytrope]] can serve as an effective surrogate for an isothermal sphere because it is infinite in extent and is dynamically unstable, but it is less cumbersome to analyze because its structure can be described by closed-form analytic expressions. + Isothermal spheres (polytropes with index $~n=\infty$) are discussed in a wide variety of astrophysical contexts because it is not uncommon for physical conditions to conspire to create an extended volume throughout which a configuration exhibits uniform temperature.  But [[User:Tohline/SSC/Structure/IsothermalSphere#Isothermal_Sphere|mathematical models of isothermal spheres]] are relatively cumbersome to analyze because they extend to infinity, they are dynamically unstable, and they are not describable in terms of analytic functions.  In such astrophysical contexts, we have sometimes found it advantageous to employ an $~n=5$ polytrope instead of an isothermal sphere.  An [[User:Tohline/SSC/Structure/Polytropes#n_.3D_5_Polytrope|isolated $~n=5$ polytrope]] can serve as an effective surrogate for an isothermal sphere because it is infinite in extent and is dynamically unstable, but it is less cumbersome to analyze because its structure can be described by closed-form analytic expressions. ==Bounded Isothermal Sphere & Bonnor-Ebert Mass== ==Bounded Isothermal Sphere & Bonnor-Ebert Mass== - In the mid-1950s, [http://adsabs.harvard.edu/abs/1955ZA.....37..217E Ebert] (1955) and [http://adsabs.harvard.edu/abs/1956MNRAS.116..351B Bonnor] (1956) independently realized that an isothermal gas cloud can be stabilized by embedding it in a hot, tenuous external medium.  The relevant mathematical model is constructed by chopping off the isothermal sphere at some finite radius — call it, $\xi_e$ — and imposing an externally applied pressure, $P_e$, that is equal to the pressure of the isothermal gas at the specified edge of the truncated sphere.  But for a given mass and temperature, there is a value of $P_e$ below which the truncated isothermal sphere is dynamically unstable, like its isolated and untruncated counterpart.  Viewed another way, given the value of $P_e$ and the isothermal sound speed, $c_s$, a bounded isothermal sphere will be dynamically stable only if its mass is below a critical value, + In the mid-1950s, [http://adsabs.harvard.edu/abs/1955ZA.....37..217E Ebert] (1955) and [http://adsabs.harvard.edu/abs/1956MNRAS.116..351B Bonnor] (1956) independently realized that an isothermal gas cloud can be stabilized by embedding it in a hot, tenuous external medium.  The relevant mathematical model is constructed by chopping off the isothermal sphere at some finite radius — call it, $~\xi_e$ — and imposing an externally applied pressure, $~P_e$, that is equal to the pressure of the isothermal gas at the specified edge of the truncated sphere.  But for a given mass and temperature, there is a value of $~P_e$ below which the truncated isothermal sphere is dynamically unstable, like its isolated and untruncated counterpart.  Viewed another way, given the value of $~P_e$ and the isothermal sound speed, $~c_s$, a bounded isothermal sphere will be dynamically stable only if its mass is below a critical value,
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- $\alpha$ + $~\alpha$
- $1.18$ + $~1.18$ Line 96: Line 96: - Bounded $n=5$ Polytrope + Bounded $~n=5$ Polytrope

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- $n=5$ Virial Analysis + $~n=5$ Virial Analysis

Line 132: Line 132: - where $\alpha$ is a dimensionless coefficient of order unity.  This limiting mass is often referred to as the Bonnor-Ebert mass.  It appears most frequently in the astrophysics literature in discussions of star formation because that is the arena in which both Bonnor and Ebert were conducting research when they made their discoveries. + where $~\alpha$ is a dimensionless coefficient of order unity.  This limiting mass is often referred to as the Bonnor-Ebert mass.  It appears most frequently in the astrophysics literature in discussions of star formation because that is the arena in which both Bonnor and Ebert were conducting research when they made their discoveries. - As is [[User:Tohline/SSC/Structure/BonnorEbert#Maximum_Mass|reviewed in a related discussion]] and as is documented in the table accompanying the expression for $M_\mathrm{max}$, above, [http://adsabs.harvard.edu/abs/1956MNRAS.116..351B Bonnor] (1956) used [[User:Tohline/SSC/Structure/IsothermalSphere#Emden.27s_Numerical_Solution|Emden's (1907) tabulated properties]] of an isothermal sphere to determine that the dimensionless radius of this limiting configuration is $\xi_e \approx 6.5$ and that the leading coefficient, $\alpha \approx 1.18$.  It is worth noting that a [[User:Tohline/SphericallySymmetricConfigurations/Virial#BonnorEbertMass|global virial analysis of the stability of bounded isothermal spheres]] produces the same expression for $M_\mathrm{max}$ with a leading coefficient that has an exact, analytic prescription, namely, $\alpha = (3^4 \cdot 5^3/2^{10}\pi)^{1/2} \approx 1.77408$.  While it can be advantageous to reference this analytic prescription of $\alpha$, the virial analysis must be considered more approximate than Bonnor's analysis because it does not require the construction of models that are in detailed force balance. + As is [[User:Tohline/SSC/Structure/BonnorEbert#Maximum_Mass|reviewed in a related discussion]] and as is documented in the table accompanying the expression for $~M_\mathrm{max}$, above, [http://adsabs.harvard.edu/abs/1956MNRAS.116..351B Bonnor] (1956) used [[User:Tohline/SSC/Structure/IsothermalSphere#Emden.27s_Numerical_Solution|Emden's (1907) tabulated properties]] of an isothermal sphere to determine that the dimensionless radius of this limiting configuration is $\xi_e \approx 6.5$ and that the leading coefficient, $\alpha \approx 1.18$.  It is worth noting that a [[User:Tohline/SphericallySymmetricConfigurations/Virial#BonnorEbertMass|global virial analysis of the stability of bounded isothermal spheres]] produces the same expression for $~M_\mathrm{max}$ with a leading coefficient that has an exact, analytic prescription, namely, $\alpha = (3^4 \cdot 5^3/2^{10}\pi)^{1/2} \approx 1.77408$.  While it can be advantageous to reference this analytic prescription of $\alpha$, the virial analysis must be considered more approximate than Bonnor's analysis because it does not require the construction of models that are in detailed force balance. - Our [[User:Tohline/SSC/Structure/PolytropesEmbedded#Extension_to_Bounded_Sphere_2|detailed force-balance analysis of truncated and pressure-bounded, $n=5$ polytropes]] identifies a physically analogous limiting mass.  If the average isothermal sound speed, $\bar{c_s}$, [[User:Tohline/SphericallySymmetricConfigurations/Virial#average|as defined elsewhere]], is used in place of $c_s$, the mathematical expression for $M_\mathrm{max}$ has exactly the same form as in the isothermal case.  But for the $n=5$ polytrope we know that the limiting configuration has a dimensionless radius given precisely by $\xi_e = 3$; and, as a result, the leading coefficient in the definition of $M_\mathrm{max}$ is prescribable analytically, namely, $\alpha = 2^{-3/10} \cdot (3^7/2^8 \pi)^{1/2} \approx 1.33943$.  As is documented in the table accompanying the relation for $M_\mathrm{max}$, above, in the case of a truncated $n=5$ polytrope, [[User:Tohline/SphericallySymmetricConfigurations/Virial#Maximum_Mass|the simpler and more approximate virial analysis gives]], $\alpha = (3^{19}/2^{12}\cdot 5^7\pi)^{1/2} \approx 1.07523$. + Our [[User:Tohline/SSC/Structure/PolytropesEmbedded#Extension_to_Bounded_Sphere_2|detailed force-balance analysis of truncated and pressure-bounded, $~n=5$ polytropes]] identifies a physically analogous limiting mass.  If the average isothermal sound speed, $~\bar{c_s}$, [[User:Tohline/SphericallySymmetricConfigurations/Virial#average|as defined elsewhere]], is used in place of $c_s$, the mathematical expression for $~M_\mathrm{max}$ has exactly the same form as in the isothermal case.  But for the $~n=5$ polytrope we know that the limiting configuration has a dimensionless radius given precisely by $~\xi_e = 3$; and, as a result, the leading coefficient in the definition of $~M_\mathrm{max}$ is prescribable analytically, namely, $~\alpha = 2^{-3/10} \cdot (3^7/2^8 \pi)^{1/2} \approx 1.33943$.  As is documented in the table accompanying the relation for $~M_\mathrm{max}$, above, in the case of a truncated $~n=5$ polytrope, [[User:Tohline/SphericallySymmetricConfigurations/Virial#Maximum_Mass|the simpler and more approximate virial analysis gives]], $~\alpha = (3^{19}/2^{12}\cdot 5^7\pi)^{1/2} \approx 1.07523$. ==Schönberg-Chandrasekhar Mass== ==Schönberg-Chandrasekhar Mass== - In the early 1940s, Chandrasekhar and his colleagues (see [http://adsabs.harvard.edu/abs/1941ApJ....94..525H Henrich & Chandraskhar (1941)] and [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)]) discovered that a star with an isothermal core will become unstable if the fractional mass of the core is above some limiting value.  They discovered this by constructing models that are now commonly referred to as bipolytropes, that is, models in which the star's core is described by a polytropic equation of state having one index — say, $n_c$ — and the star's envelope is described by a polytropic equation of state of a different index — say, $n_e$.  In [[User:Tohline/SSC/Structure/BiPolytropes#BiPolytropes|an accompanying discussion]] we explain in detail how the two structural components with different polytropic indexes are pieced together mathematically to build equilibrium bipolytropes. For a given choice of the two indexes, $n_c$ and $n_e$, a sequence of models can be generated by varying the radial location at which the interface between the core and envelope occurs.  As the interface location is varied, the relative amount of mass enclosed inside the core, $\nu \equiv M_\mathrm{core}/M_\mathrm{tot}$, quite naturally varies as well. + In the early 1940s, Chandrasekhar and his colleagues (see [http://adsabs.harvard.edu/abs/1941ApJ....94..525H Henrich & Chandraskhar (1941)] and [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)]) discovered that a star with an isothermal core will become unstable if the fractional mass of the core is above some limiting value.  They discovered this by constructing models that are now commonly referred to as ''composite polytropes'' or ''bipolytropes'', that is, models in which the star's core is described by a polytropic equation of state having one index — say, $~n_c$ — and the star's envelope is described by a polytropic equation of state of a different index — say, $~n_e$.  In [[User:Tohline/SSC/Structure/BiPolytropes#BiPolytropes|an accompanying discussion]] we explain in detail how the two structural components with different polytropic indexes are pieced together mathematically to build equilibrium bipolytropes. For a given choice of the two indexes, $~n_c$ and $~n_e$, a sequence of models can be generated by varying the radial location at which the interface between the core and envelope occurs.  As the interface location is varied, the relative amount of mass enclosed inside the core, $~\nu \equiv M_\mathrm{core}/M_\mathrm{tot}$, quite naturally varies as well. - [http://adsabs.harvard.edu/abs/1941ApJ....94..525H Henrich & Chandraskhar (1941)] built structures of uniform composition having an isothermal core ($n_c = \infty$) and an $n_e = 3/2$ polytropic envelope and found that equilibrium models exist only for values of $\nu \le \nu_\mathrm{max} \approx 0.35$.  [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)] extended this analysis to include structures in which the mean molecular weight of the gas changes discontinuously across the interface.  Specifically, they used the same values of $n_c$ and $n_e$ as Henrich & Chandrasekhar, but they constructed models in which the ratio of the molecular weight in the core to the molecular weight in the envelope is $\mu_c/\mu_e = 2$. This was done to more realistically represent stars as they evolve off the main sequence; they have inert, isothermal helium cores and envelopes that are rich in hydrogen.  Note that introducing a discontinuous drop in the mean molecular weight at the core-envelope interface also introduces a discontinuous drop in the gas density across the interface.  As the following excerpt from p. 168 of their article summarizes, in these models, [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)] found that $\nu_\mathrm{max} \approx 0.101$.  This is commonly referred to as the Schönberg-Chandrasekhar mass limit, although it was Henrich & Chandrasekhar who were the first to identify the instability. + [http://adsabs.harvard.edu/abs/1941ApJ....94..525H Henrich & Chandraskhar (1941)] built structures of uniform composition having an isothermal core ($~n_c = \infty$) and an $~n_e = 3/2$ polytropic envelope and found that equilibrium models exist only for values of $~\nu \le \nu_\mathrm{max} \approx 0.35$.  [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)] extended this analysis to include structures in which the mean molecular weight of the gas changes discontinuously across the interface.  Specifically, they used the same values of $~n_c$ and $~n_e$ as Henrich & Chandrasekhar, but they constructed models in which the ratio of the molecular weight in the core to the molecular weight in the envelope is $~\mu_c/\mu_e = 2$. This was done to more realistically represent stars as they evolve off the main sequence; they have inert, isothermal helium cores and envelopes that are rich in hydrogen.  Note that introducing a discontinuous drop in the mean molecular weight at the core-envelope interface also introduces a discontinuous drop in the gas density across the interface.  As the following excerpt from p. 168 of their article summarizes, in these models, [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)] found that $~\nu_\mathrm{max} \approx 0.101$.  This is commonly referred to as the Schönberg-Chandrasekhar mass limit, although it was Henrich & Chandrasekhar who were the first to identify the instability.
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[[Image:SC42excerpt.jpg|600px|center]] [[Image:SC42excerpt.jpg|600px|center]] +
- In an effort to develop a more complete appreciation of the onset of the instability associated with the Schönberg-Chandrasekhar mass limit, [http://adsabs.harvard.edu/abs/1988Ap%26SS.147..219B Beech (1988)] matched an analytically prescribable, $n_e = 1$ polytropic envelope to an isothermal core and, like Schönberg & Chandrasekhar, allowed for a discontinuous change in the molecular weight at the interface.  His results were not significantly different from those reported by [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)]; in particular, the value of $\nu_\mathrm{max}$ was still only definable numerically because an isothermal core cannot be described in terms of analytic functions. + In an effort to develop a more complete appreciation of the onset of the instability associated with the Schönberg-Chandrasekhar mass limit, [http://adsabs.harvard.edu/abs/1988Ap%26SS.147..219B Beech (1988)] matched an analytically prescribable, $~n_e = 1$ polytropic envelope to an isothermal core and, like Schönberg & Chandrasekhar, allowed for a discontinuous change in the molecular weight at the interface.  [For an even more comprehensive generalization and discussion, see [http://adsabs.harvard.edu/abs/2012MNRAS.421.2713B Ball, Tout, & Żytkow] (2012, MNRAS, 421, 2713)].  Beech's results were not significantly different from those reported by [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)]; in particular, the value of $~\nu_\mathrm{max}$ was still only definable numerically because an isothermal core cannot be described in terms of analytic functions. - [[User:Tohline/SSC/Structure/BiPolytropes/Analytic5_1#BiPolytrope_with_nc_.3D_5_and_ne_.3D_1|In an accompanying derivation]] we have gone one step farther, matching an analytically prescribable, $n_e = 1$ polytropic envelope to an analytically prescribable, $n_c = 5$ polytropic core.  For this bipolytrope, we show that there is a limiting mass-fraction, $\nu_\mathrm{max}$, for any choice of the molecular weight ratio $\mu_c/\mu_e > 3$ and that the interface location, $\xi_i$, associated with this critical configuration is given by the positive, real root of the following relation: + [[User:Tohline/SSC/Structure/BiPolytropes/Analytic5_1#BiPolytrope_with_nc_.3D_5_and_ne_.3D_1|In an accompanying derivation]] [see, also, [http://adsabs.harvard.edu/abs/1998MNRAS.298..831E Eggleton, Faulkner, and Cannon] (1998, MNRAS, 298, 831)] we have gone one step farther, matching an analytically prescribable, $~n_e = 1$ polytropic envelope to an analytically prescribable, $~n_c = 5$ polytropic core.  For this bipolytrope, we show that there is a limiting mass-fraction, $~\nu_\mathrm{max}$, for any choice of the molecular weight ratio $~\mu_c/\mu_e > 3$ and that the interface location, $~\xi_i$, associated with this critical configuration is given by the positive, real root of the following relation:
Line 186: Line 187: ==Relationship Between the Bonnor-Ebert and Schönberg-Chandrasekhar Critical Masses== ==Relationship Between the Bonnor-Ebert and Schönberg-Chandrasekhar Critical Masses== - [[User:Tohline/SSC/Structure/BiPolytropes/Analytic5_1#Limit_when_m3_.3D_0|As we have shown elsewhere]], in the limit $m_3 \rightarrow 0$, the physically relevant root of the above analytic relation is $\xi_i = 3$ and the mass contained in the core is, + [[User:Tohline/SSC/Structure/BiPolytropes/Analytic5_1#Limit_when_m3_.3D_0|As we have shown elsewhere]], in the limit $~m_3 \rightarrow 0$, the physically relevant root of the above analytic relation is $~\xi_i = 3$ and the mass contained in the core is,
$[itex] M_\mathrm{core} = \biggl( \frac{1}{2} \biggr)^{3/10}\biggl( \frac{3^{7}}{2^{8}\pi} \biggr)^{1/2} \biggl( \frac{c_s^8}{G^3 P_e} \biggr)^{1/2} \, .$ M_\mathrm{core} = \biggl( \frac{1}{2} \biggr)^{3/10}\biggl( \frac{3^{7}}{2^{8}\pi} \biggr)^{1/2} \biggl( \frac{c_s^8}{G^3 P_e} \biggr)^{1/2} \, .[/itex]
- While the pressure at the base of the envelope in this model is satisfactorily confining the core to a finite radius, the condition $m_3 \rightarrow 0$ implies that the mass-density at the base of — indeed, throughout — the envelope is zero.  [[User:Tohline/SSC/Structure/BiPolytropes#The_Tohline_Generalization|As we have pointed out elsewhere]], this can be achieved by introducing a temperature discontinuity rather than a molecular weight discontinuity across the interface.  Hence, there is no mass in the envelope and the resulting model is, effectively, a truncated $n=5$ polytrope embedded in a hot, tenuous external medium.  It therefore should not come as a surprise that this critical Schönberg-Chandrasekhar-type configuration has a mass that is precisely equal to the Bonnor-Ebert limiting mass, as defined by a "bounded $n=5$ polytrope."  (See the second row from the bottom in the above table.) + While the pressure at the base of the envelope in this model is satisfactorily confining the core to a finite radius, the condition $~m_3 \rightarrow 0$ implies that the mass-density at the base of — indeed, throughout — the envelope is zero.  [[User:Tohline/SSC/Structure/BiPolytropes#The_Tohline_Generalization|As we have pointed out elsewhere]], this can be achieved by introducing a temperature discontinuity rather than a molecular weight discontinuity across the interface.  Hence, there is no mass in the envelope and the resulting model is, effectively, a truncated $~n=5$ polytrope embedded in a hot, tenuous external medium.  It therefore should not come as a surprise that this critical Schönberg-Chandrasekhar-type configuration has a mass that is precisely equal to the Bonnor-Ebert limiting mass, as defined by a "bounded $~n=5$ polytrope."  (See the second row from the bottom in the above table.) It should be clear from this analysis that the Bonnor-Ebert critical mass is not distinct from the Schönberg-Chandrasekhar critical mass.  It can be derived from the Schönberg-Chandrasekhar mass in the limit when $\mu_e/\mu_c \rightarrow 0$.  Had [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)] examined their model in this limit, they would have "discovered" the Bonnor-Ebert mass a decade prior to both Bonnor's and Ebert's published works. It should be clear from this analysis that the Bonnor-Ebert critical mass is not distinct from the Schönberg-Chandrasekhar critical mass.  It can be derived from the Schönberg-Chandrasekhar mass in the limit when $\mu_e/\mu_c \rightarrow 0$.  Had [http://adsabs.harvard.edu/abs/1942ApJ....96..161S Schönberg & Chandrasekhar (1942)] examined their model in this limit, they would have "discovered" the Bonnor-Ebert mass a decade prior to both Bonnor's and Ebert's published works. Line 207: Line 208:
[[File:Stahler1983TitlePage0.png|300px|center|Stahler (1983) Title Page]] [[File:Stahler1983TitlePage0.png|300px|center|Stahler (1983) Title Page]] + Line 216: Line 218: [[File:Stahler_MRdiagram1.png|300px|center|Stahler (1983) Figure 17 (edited)]] [[File:Stahler_MRdiagram1.png|300px|center|Stahler (1983) Figure 17 (edited)]] + Line 242: Line 245: * [[User:Tohline/SSC/Structure/LimitingMasses#Sch.C3.B6nberg-Chandrasekhar_Mass|Schönberg-Chandrasekhar limiting mass]] * [[User:Tohline/SSC/Structure/LimitingMasses#Sch.C3.B6nberg-Chandrasekhar_Mass|Schönberg-Chandrasekhar limiting mass]] * [[User:Tohline/SSC/Structure/LimitingMasses#Relationship_Between_the_Bonnor-Ebert_and_Sch.C3.B6nberg-Chandrasekhar_Critical_Masses|Relationship between Bonnor-Ebert and Schönberg-Chandrasekhar limiting masses]] * [[User:Tohline/SSC/Structure/LimitingMasses#Relationship_Between_the_Bonnor-Ebert_and_Sch.C3.B6nberg-Chandrasekhar_Critical_Masses|Relationship between Bonnor-Ebert and Schönberg-Chandrasekhar limiting masses]] + * [https://ui.adsabs.harvard.edu/abs/1971A%26A....14..351M/abstract Maeder, A. (1971, Astron. & Astrophysics, 14, 351 - 358).] — Examines the effects of rotation on the Schönberg-Chandrasekhar limiting mass. {{LSU_HBook_footer}} {{LSU_HBook_footer}}
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# Mass Upper Limits

Spherically symmetric, self-gravitating, equilibrium configurations can be constructed from gases exhibiting a wide variety of degrees of compressibility. When examining how the internal structure of such configurations varies with compressibility, or when examining the relative stability of such structures, it can be instructive to construct models using a polytropic equation of state because the degree of compressibility can be adjusted by simply changing the value of the polytropic index, $~n$, across the range, $~0 \le n \le \infty$. (Alternatively, one can vary the effective adiabatic exponent of the gas, $~\gamma_g = 1 + 1/n$.) In particular, $~n = 0 ~~ (\gamma_g = \infty)$ represents a hard equation of state and describes an incompressible configuration, while $~n = \infty ~~(\gamma_g = 1)$ represents an isothermal and extremely soft equation of state.

## Isolated Polytropes

Isolated polytropic spheres exhibit three attributes that are especially key in the context of our present discussion:

1. The equilibrium structure is dynamically stable if $~n < 3$.
2. The equilibrium structure has a finite radius if $~n < 5$.
3. The equilibrium structure can be described in terms of closed-form analytic expressions for $~n = 0$, $~n = 1$, and $~n = 5$.

## Isothermal Spheres

Isothermal spheres (polytropes with index $~n=\infty$) are discussed in a wide variety of astrophysical contexts because it is not uncommon for physical conditions to conspire to create an extended volume throughout which a configuration exhibits uniform temperature. But mathematical models of isothermal spheres are relatively cumbersome to analyze because they extend to infinity, they are dynamically unstable, and they are not describable in terms of analytic functions. In such astrophysical contexts, we have sometimes found it advantageous to employ an $~n=5$ polytrope instead of an isothermal sphere. An isolated $~n=5$ polytrope can serve as an effective surrogate for an isothermal sphere because it is infinite in extent and is dynamically unstable, but it is less cumbersome to analyze because its structure can be described by closed-form analytic expressions.

## Bounded Isothermal Sphere & Bonnor-Ebert Mass

In the mid-1950s, Ebert (1955) and Bonnor (1956) independently realized that an isothermal gas cloud can be stabilized by embedding it in a hot, tenuous external medium. The relevant mathematical model is constructed by chopping off the isothermal sphere at some finite radius — call it, $~\xi_e$ — and imposing an externally applied pressure, $~P_e$, that is equal to the pressure of the isothermal gas at the specified edge of the truncated sphere. But for a given mass and temperature, there is a value of $~P_e$ below which the truncated isothermal sphere is dynamically unstable, like its isolated and untruncated counterpart. Viewed another way, given the value of $~P_e$ and the isothermal sound speed, $~c_s$, a bounded isothermal sphere will be dynamically stable only if its mass is below a critical value,

Bonnor-Ebert Mass

$M_\mathrm{max} = \alpha \biggl( \frac{c_s^8}{G^3 P_e} \biggr)^{1/2}$

Coefficient α for Pressure-Bounded Configurations

$~\alpha$

Context

Source

$~1.18$

Bounded Isothermal Sphere
(numerically derived)

Discovery Paper
Bonnor (1956)

$\biggl( \frac{3^4\cdot 5^3}{2^{10}\pi} \biggr)^{1/2}$

Isothermal Virial Analysis
(exact)

$\biggl( \frac{1}{2} \biggr)^{3/10}\biggl( \frac{3^{7}}{2^{8}\pi} \biggr)^{1/2}$

Bounded $~n=5$ Polytrope
(exact)

$\biggl( \frac{3^{19}}{2^{12}\cdot 5^7\pi} \biggr)^{1/2}$

$~n=5$ Virial Analysis
(exact)

where $~\alpha$ is a dimensionless coefficient of order unity. This limiting mass is often referred to as the Bonnor-Ebert mass. It appears most frequently in the astrophysics literature in discussions of star formation because that is the arena in which both Bonnor and Ebert were conducting research when they made their discoveries.

As is reviewed in a related discussion and as is documented in the table accompanying the expression for $~M_\mathrm{max}$, above, Bonnor (1956) used Emden's (1907) tabulated properties of an isothermal sphere to determine that the dimensionless radius of this limiting configuration is $\xi_e \approx 6.5$ and that the leading coefficient, $\alpha \approx 1.18$. It is worth noting that a global virial analysis of the stability of bounded isothermal spheres produces the same expression for $~M_\mathrm{max}$ with a leading coefficient that has an exact, analytic prescription, namely, $\alpha = (3^4 \cdot 5^3/2^{10}\pi)^{1/2} \approx 1.77408$. While it can be advantageous to reference this analytic prescription of α, the virial analysis must be considered more approximate than Bonnor's analysis because it does not require the construction of models that are in detailed force balance.

Our detailed force-balance analysis of truncated and pressure-bounded, $~n=5$ polytropes identifies a physically analogous limiting mass. If the average isothermal sound speed, $~\bar{c_s}$, as defined elsewhere, is used in place of cs, the mathematical expression for $~M_\mathrm{max}$ has exactly the same form as in the isothermal case. But for the $~n=5$ polytrope we know that the limiting configuration has a dimensionless radius given precisely by $~\xi_e = 3$; and, as a result, the leading coefficient in the definition of $~M_\mathrm{max}$ is prescribable analytically, namely, $~\alpha = 2^{-3/10} \cdot (3^7/2^8 \pi)^{1/2} \approx 1.33943$. As is documented in the table accompanying the relation for $~M_\mathrm{max}$, above, in the case of a truncated $~n=5$ polytrope, the simpler and more approximate virial analysis gives, $~\alpha = (3^{19}/2^{12}\cdot 5^7\pi)^{1/2} \approx 1.07523$.

## Schönberg-Chandrasekhar Mass

In the early 1940s, Chandrasekhar and his colleagues (see Henrich & Chandraskhar (1941) and Schönberg & Chandrasekhar (1942)) discovered that a star with an isothermal core will become unstable if the fractional mass of the core is above some limiting value. They discovered this by constructing models that are now commonly referred to as composite polytropes or bipolytropes, that is, models in which the star's core is described by a polytropic equation of state having one index — say, $~n_c$ — and the star's envelope is described by a polytropic equation of state of a different index — say, $~n_e$. In an accompanying discussion we explain in detail how the two structural components with different polytropic indexes are pieced together mathematically to build equilibrium bipolytropes. For a given choice of the two indexes, $~n_c$ and $~n_e$, a sequence of models can be generated by varying the radial location at which the interface between the core and envelope occurs. As the interface location is varied, the relative amount of mass enclosed inside the core, $~\nu \equiv M_\mathrm{core}/M_\mathrm{tot}$, quite naturally varies as well.

Henrich & Chandraskhar (1941) built structures of uniform composition having an isothermal core ($~n_c = \infty$) and an $~n_e = 3/2$ polytropic envelope and found that equilibrium models exist only for values of $~\nu \le \nu_\mathrm{max} \approx 0.35$. Schönberg & Chandrasekhar (1942) extended this analysis to include structures in which the mean molecular weight of the gas changes discontinuously across the interface. Specifically, they used the same values of $~n_c$ and $~n_e$ as Henrich & Chandrasekhar, but they constructed models in which the ratio of the molecular weight in the core to the molecular weight in the envelope is $~\mu_c/\mu_e = 2$. This was done to more realistically represent stars as they evolve off the main sequence; they have inert, isothermal helium cores and envelopes that are rich in hydrogen. Note that introducing a discontinuous drop in the mean molecular weight at the core-envelope interface also introduces a discontinuous drop in the gas density across the interface. As the following excerpt from p. 168 of their article summarizes, in these models, Schönberg & Chandrasekhar (1942) found that $~\nu_\mathrm{max} \approx 0.101$. This is commonly referred to as the Schönberg-Chandrasekhar mass limit, although it was Henrich & Chandrasekhar who were the first to identify the instability.

 Text excerpt from Schönberg & Chandrasekhar (1942)

In an effort to develop a more complete appreciation of the onset of the instability associated with the Schönberg-Chandrasekhar mass limit, Beech (1988) matched an analytically prescribable, $~n_e = 1$ polytropic envelope to an isothermal core and, like Schönberg & Chandrasekhar, allowed for a discontinuous change in the molecular weight at the interface. [For an even more comprehensive generalization and discussion, see Ball, Tout, & Żytkow (2012, MNRAS, 421, 2713)]. Beech's results were not significantly different from those reported by Schönberg & Chandrasekhar (1942); in particular, the value of $~\nu_\mathrm{max}$ was still only definable numerically because an isothermal core cannot be described in terms of analytic functions.

In an accompanying derivation [see, also, Eggleton, Faulkner, and Cannon (1998, MNRAS, 298, 831)] we have gone one step farther, matching an analytically prescribable, $~n_e = 1$ polytropic envelope to an analytically prescribable, $~n_c = 5$ polytropic core. For this bipolytrope, we show that there is a limiting mass-fraction, $~\nu_\mathrm{max}$, for any choice of the molecular weight ratio $~\mu_c/\mu_e > 3$ and that the interface location, $~\xi_i$, associated with this critical configuration is given by the positive, real root of the following relation:

$\biggl(\frac{\pi}{2} + \tan^{-1} \Lambda_i\biggr) (1+\ell_i^2) [ 3 + (1-m_3)^2(2-\ell_i^2)\ell_i^2] - m_3 \ell_i [(1-m_3)\ell_i^4 - (m_3^2 - m_3 +2)\ell_i^2 - 3] = 0 \, ,$

where,

$\ell_i \equiv \frac{\xi_i}{\sqrt{3}} \, ;$             $m_3 \equiv 3 \biggl( \frac{\mu_c}{\mu_e} \biggr)^{-1} \, ;$       and       $\Lambda_i \equiv \frac{1}{m_3\ell_i} [ 1 + (1-m_3)\ell_i^2] \, .$

## Relationship Between the Bonnor-Ebert and Schönberg-Chandrasekhar Critical Masses

As we have shown elsewhere, in the limit $~m_3 \rightarrow 0$, the physically relevant root of the above analytic relation is $~\xi_i = 3$ and the mass contained in the core is,

$M_\mathrm{core} = \biggl( \frac{1}{2} \biggr)^{3/10}\biggl( \frac{3^{7}}{2^{8}\pi} \biggr)^{1/2} \biggl( \frac{c_s^8}{G^3 P_e} \biggr)^{1/2} \, .$

While the pressure at the base of the envelope in this model is satisfactorily confining the core to a finite radius, the condition $~m_3 \rightarrow 0$ implies that the mass-density at the base of — indeed, throughout — the envelope is zero. As we have pointed out elsewhere, this can be achieved by introducing a temperature discontinuity rather than a molecular weight discontinuity across the interface. Hence, there is no mass in the envelope and the resulting model is, effectively, a truncated $~n=5$ polytrope embedded in a hot, tenuous external medium. It therefore should not come as a surprise that this critical Schönberg-Chandrasekhar-type configuration has a mass that is precisely equal to the Bonnor-Ebert limiting mass, as defined by a "bounded $~n=5$ polytrope." (See the second row from the bottom in the above table.)

It should be clear from this analysis that the Bonnor-Ebert critical mass is not distinct from the Schönberg-Chandrasekhar critical mass. It can be derived from the Schönberg-Chandrasekhar mass in the limit when $\mu_e/\mu_c \rightarrow 0$. Had Schönberg & Chandrasekhar (1942) examined their model in this limit, they would have "discovered" the Bonnor-Ebert mass a decade prior to both Bonnor's and Ebert's published works.

Material that appears after this point in our presentation is under development and therefore
may contain incorrect mathematical equations and/or physical misinterpretations.
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