source
stringlengths 1
2.05k
⌀ | target
stringlengths 1
11.7k
|
|---|---|
Both phenomena may occur together. where usually the high-velocity jet is enclosed. in a low-velocity molecular outflow. | Both phenomena may occur together, where usually the high-velocity jet is enclosed in a low-velocity molecular outflow. |
The physical mechanisms that drive outllows are still not Cully understood. | The physical mechanisms that drive outflows are still not fully understood. |
The adiabatic (or ‘lirst’) core. the circumstellar disc around the protostar and the protostar itself are. possible origins of either jet or molecular outllow or both. | The adiabatic (or 'first') core, the circumstellar disc around the protostar and the protostar itself are possible origins of either jet or molecular outflow or both. |
First analvtical work bv? and 7? suggested rapid rotating. magnetised: protostellar. cliscs as possible origins of these outllows. since other sources like pressure due to either the gas or radiation. have been ruled: out since those mechanisms fail to provide sullicient energv and momentum. | First analytical work by \cite{Blandford1982fk} and \cite{Pudritz1983uq} suggested rapid rotating, magnetised protostellar discs as possible origins of these outflows, since other sources like pressure due to either the gas or radiation, have been ruled out since those mechanisms fail to provide sufficient energy and momentum. |
Later. ?? introduced the idea of a magnetic tower’. an outflow driven by magnetic pressure originating in toroidal magnetic field colupiHens. | Later, \cite{Lynden-Bell1996fk,Lynden-Bell2003fk} introduced the idea of a 'magnetic tower', an outflow driven by magnetic pressure originating in toroidal magnetic field components. |
From a numerical point of view. the simulation hy ? was one of the first to produce a magnetically driven outfTow cluring the collapse of a maenetisecl anc| rotating molecular cloud core. | From a numerical point of view, the simulation by \cite{Tomisaka1998fk} was one of the first to produce a magnetically driven outflow during the collapse of a magnetised and rotating molecular cloud core. |
Phere it was shown that the outflow is launched by clynamically buildinο up of a toroidal magnetic. field. | There it was shown that the outflow is launched by dynamically building up of a toroidal magnetic field. |
Other simulations concentrating on outllow phenomena were performed. by ο οι, and 7? who follow«d the evolution up | Other simulations concentrating on outflow phenomena were performed by \cite{Tomisaka2000fj,Tomisaka2002kx}, , and \cite{Banerjee2006uq} who followed the evolution up |
brightest two PNe SMP77 and SMP78 from our calibrator list and safely assume that the continuum contributions for MG60, MG65 and Sal22 are smaller than the errors (0.2 dex). | brightest two PNe SMP77 and SMP78 from our calibrator list and safely assume that the continuum contributions for MG60, MG65 and Sa122 are smaller than the errors (0.2 dex). |
We also excluded MG68 which was found to not fit the trend (see below). | We also excluded MG68 which was found to not fit the trend (see below). |
Figure 4 shows the derived calibration after application of a linear least squares fit. | Figure \ref{fig:fit} shows the derived calibration after application of a linear least squares fit. |
The well-behaved trend is a testament to the careful [O III] flux measurements performed by RP2010. | The well-behaved trend is a testament to the careful [O III] flux measurements performed by RP2010. |
The fluxes in Tab. | The fluxes in Tab. |
2 were derived from the fit after measuring their counts and have an associated uncertainty of 0.07 dex from the standard error of the fit. | \ref{tab:new} were derived from the fit after measuring their counts and have an associated uncertainty of 0.07 dex from the standard error of the fit. |
This value is also twice the measured c from the fit-subtracted residuals. | This value is also twice the measured $\sigma$ from the fit-subtracted residuals. |
Jacoby (1989) Msoo7 magnitudes suitable for the PNLF were also calculated as usual via the relation 7599;=—2.5logFsoo;—13.74 and placed in Tab. 2.. | Jacoby (1989) $m_{5007}$ magnitudes suitable for the PNLF were also calculated as usual via the relation $m_{5007}=-2.5 \log F_{5007} - 13.74$ and placed in Tab. \ref{tab:new}. |
MG68 was excluded from the fit because its published flux falls 2σ (0.4 dex) lower than the expected value of log Fs5og;=—12.74+0.07 dex. | MG68 was excluded from the fit because its published flux falls $\sigma$ (0.4 dex) lower than the expected value of log $_{5007}=-12.74\pm0.07$ dex. |
This may be explained by either (a) the non-photometric conditions of the data, or (b) a real underestimation by RP2010. | This may be explained by either (a) the non-photometric conditions of the data, or (b) a real underestimation by RP2010. |
It does not seem possible to distinguish between the two as there are no other calibrator PNe besides MG68 in the 30Dor1 sub-field. | It does not seem possible to distinguish between the two as there are no other calibrator PNe besides MG68 in the 30Dor1 sub-field. |
If (b) is true, then this could be explained by the strong spatial variation of [O III] in MG68 which is not accommodated by the small ffibre aperture of RP2010 (see Miszalski et al. | If (b) is true, then this could be explained by the strong spatial variation of [O III] in MG68 which is not accommodated by the small fibre aperture of RP2010 (see Miszalski et al. |
2011). | 2011). |
therefore (A2) implies: Using €CA7)). the system (A5)) can be transformed into: This sytem can be solved by successive approximations. | therefore \ref{eq:Flaw}) ) implies: Using \ref{eq:dB}) ), the system \ref{eq:mom1}) ) can be transformed into: This sytem can be solved by successive approximations. |
For instance the ratio: since Ja.)~Ty: By=Ba/γπρι represents the Alfvénn velocity (as measured in the upstream rest frame). | For instance the ratio: since $\vert u_x\vert\sim\Gamma_{\rm sh}$; $\beta_{\rm A}=B_{y|u}/\sqrt{4\pi \rho_u c^2}$ represents the Alfvénn velocity (as measured in the upstream rest frame). |
Hence: Consider now the ratio of the first term on the Ihs of the second equation in CAS) to the term of the rhs of the same equation: | Hence: Consider now the ratio of the first term on the lhs of the second equation in \ref{eq:mom2}) ) to the term of the rhs of the same equation: This ratio is much smaller than unity (since $u_z\,\ll\,\Gamma_{\rm
sh}$ ). |
In the last equation. x; corresponds to the maximal distance to which cosmic rays can stream ahead of the shock front. as measured in the shock front frame. | Then: In the last equation, $x_*$ corresponds to the maximal distance to which cosmic rays can stream ahead of the shock front, as measured in the shock front frame. |
We also assume that εν. B, and p vary on much longer scales than Π.. and that [i|«[i]. | We also assume that $u_x$, $B_y$ and $\rho$ vary on much longer scales than $u_z$, and that $\vert
u_z\vert\ll\vert u_x\vert$. |
This hierarchy ean be veritied by taking the ratios of the equations in CAS»). | This hierarchy can be verified by taking the ratios of the equations in \ref{eq:mom1}) ). |
Since Bz/Gbry)xB.Fy. one can simplify the previous expression and obtain the following order of magnitude: To obtain this result. we have approximated the integral over Po US Eso. € representing the length scale of the distribution in the shock frame. and written po=e,/(Gck e denotes the cosmic ray energy density while p. G1.) represents their typical momentum (Larmor radius). | Since $B_y^2/(4\pi\gamma)\,\approx\,\beta_{\rm A}^2 F_{\rm m}$, one can simplify the previous expression and obtain the following order of magnitude: To obtain this result, we have approximated the integral over $\rho_{\rm cr}$ as $\ell_{\rm cr}\rho_{\rm cr}$, $\ell_{\rm cr}$ representing the length scale of the distribution in the shock frame, and written $\rho_{\rm cr}\simeq e_{\rm cr}/(p_*c)$; $e_{\rm cr}$ denotes the cosmic ray energy density while $p_*$ $r_{\rm L *}$ ) represents their typical momentum (Larmor radius). |
Finally. ον...Tyé where £4 is the fraction of shock internal energy carried away by the accelerated population. | Finally, $e_{\rm
cr}/(\Gamma_{\rm sh}\rho_{\rm u}c^2)\,\sim\,\Gamma_{\rm sh}\xi_{\rm
cr}$ where $\xi_{\rm cr}$ is the fraction of shock internal energy carried away by the accelerated population. |
In a straightforward way. one obtains: so that: This justities the previous approximations. | In a straightforward way, one obtains: so that: This justifies the previous approximations. |
The perturbed Ohm law leads to: We keep track of the terms in zu. in these equations in order to properly evaluate the terms which involve the derivative of n. with respect to x. | The perturbed Ohm law leads to: We keep track of the terms in $u_z$ in these equations in order to properly evaluate the terms which involve the derivative of $u_z$ with respect to $x$. |
This latter quantity is of the same order than other background quantities and cannot be neglected. | This latter quantity is of the same order than other background quantities and cannot be neglected. |
However. terms in u- will be neglected in the final equations of evolution of the various background quantities since i.« | However, terms in $u_z$ will be neglected in the final equations of evolution of the various background quantities since $u_z\ll u_x$. |
For similar reasons. derivatives of background quantities (other than n) such as py. B, and a, (hence y) can be neglected. | For similar reasons, derivatives of background quantities (other than $u_z$ ) such as $\rho_{\rm pl}$, $B_y$ and $u_x$ (hence $\gamma$ ) can be neglected. |
Thus. setting y=Ty. 6=Py we obtain: The perturbed equations for the perturbed components of the magnetic field. defined in units of B, as b=0B/B, can be written: The continuity equation can be expressed as: We have noted w=p,c the proper enthalpy density of the upstream plasma. | Thus, setting $\gamma \simeq \Gamma_{\rm sh}$, $\beta
\simeq \beta_{\rm sh}$ we obtain: The perturbed equations for the perturbed components of the magnetic field, defined in units of $B_y$ as $\mathbf{b}=\mathbf{\delta
B}/B_y$ can be written: The continuity equation can be expressed as: We have noted $w = \rho_u c^2$ the proper enthalpy density of the upstream plasma. |
In the perturbation regime the contribution of the temporal derivative of the fluctuating part of the Lorentz factor | In the perturbation regime the contribution of the temporal derivative of the fluctuating part of the Lorentz factor |
in the profiles plus any stochastic instabilities of the wind. | in the profiles plus any stochastic instabilities of the wind. |
New monitoring with much higher S/N may allow Νας. multimode pulsations ancl clearly separate a sinusoidal curve of the radial pulsations to be revealed. | New monitoring with much higher S/N may allow NRPs, multimode pulsations and clearly separate a sinusoidal curve of the radial pulsations to be revealed. |
Llowever. we found convincing evidence that the atmospheric motions cannot be ascribed. solely to Ixeplerian. motions and. probably are not of a binary origin. | However, we found convincing evidence that the atmospheric motions cannot be ascribed solely to Keplerian motions and probably are not of a binary origin. |
We thank D. Baade. O. Pols and Pablo Itodriguez for their useful comments. | We thank D. Baade, O. Pols and Pablo Rodriguez for their useful comments. |
A. €. thanks the Canadian Astronomical Society Dor the travel grant to SAO. and. 1. Jikmaey for helpful discussions. | A. G. thanks the Canadian Astronomical Society for the travel grant to SAO, and I. Bikmaev for helpful discussions. |
We wish to thank the anonymous referee for his careful reading of the manuscript and several COnDslructive suggestions. | We wish to thank the anonymous referee for his careful reading of the manuscript and several constructive suggestions. |
Although X-rav imaging has allowed us to observe the morphology of the radiation emitted by accelerated particles. it remains of interest to measure the spatially integrated emission from the shock region. which often is (he only quantity we can actually measure. | Although X-ray imaging has allowed us to observe the morphology of the radiation emitted by accelerated particles, it remains of interest to measure the spatially integrated emission from the shock region, which often is the only quantity we can actually measure. |
In (his section we discuss our results for the spatially integrated spectra of accelerated. particles. which have a behavior similar to that of the integrated emission. | In this section we discuss our results for the spatially integrated spectra of accelerated particles, which have a behavior similar to that of the integrated emission. |
The spatially integrated spectra can be obtained by integrating Eqs. | The spatially integrated spectra can be obtained by integrating Eqs. |
7 and 8 in vr in the appropriate regions upstream and downstream. namely: Alter caleulating analytically the integral over cé we obtain: in the same wav. the integral over the downstream region reads: Gof) llere Erf(y) is the error [unction. | \ref{eq:N1} and \ref{eq:N2} in $x$ in the appropriate regions upstream and downstream, namely: After calculating analytically the integral over $x$ we obtain: Proceeding in the same way, the integral over the downstream region reads: Here $Erf(y)$ is the error function. |
These expressions apply to anv choice of the momentum dependence of the dilfusion | These expressions apply to any choice of the momentum dependence of the diffusion |
distributions (SEDs). | distributions (SEDs). |
We will also separately consider the possibility that 7y is elevated in the four southern clumps SMM I-4. | We will also separately consider the possibility that $T_{\rm d}$ is elevated in the four southern clumps SMM 1–4. |
The MSX. IRAS. LABOCA. and SIMBA data were used to fit the spectral energy distributions (SEDs) of IRAS 13037-6112 and IRAS 13039-6108. | The MSX, IRAS, LABOCA, and SIMBA data were used to fit the spectral energy distributions (SEDs) of IRAS 13037-6112 and IRAS 13039-6108. |
The SIMBA 1.2 mm flux densities of these sources are 0.89 and 1.36 Jy. respectively (Beltranetal.2006:: Table 2 therein). | The SIMBA 1.2 mm flux densities of these sources are 0.89 and 1.36 Jy, respectively \cite{beltran2006}; Table 2 therein). |
Note that there is not enough data points for IRAS 13042-6105 in order to construct a reasonable SED (e.g.. most of its IRAS flux densities are only upper limits. see Table 3)) | Note that there is not enough data points for IRAS 13042-6105 in order to construct a reasonable SED (e.g., most of its IRAS flux densities are only upper limits, see Table \ref{table:IRAS}) ). |
The derived SEDs are shown in Fig. 5.. | The derived SEDs are shown in Fig. \ref{figure:sed}. |
The least-squares fitting routine used in the derivation of the minimises the sum X?-log(saa. where N is the number oflogis data (sect)points (7 and 8 for IRAS 13037-6112 and 13039-6108. respectively). $?Gl) is the observed flux density. and S60) is the model flux density. | The least-squares fitting routine used in the derivation of the minimises the sum $\sum_{i=1}^N \left[\log_{10}\left(S_{\nu}^{\rm obs}(\lambda_i)\right)-\log_{10}\left(S_{\nu}^{\rm mod}(\lambda_i)\right)\right]^2$, where $N$ is the number of data points (7 and 8 for IRAS 13037-6112 and 13039-6108, respectively), $S_{\nu}^{\rm obs}(\lambda_i)$ is the observed flux density, and $S_{\nu}^{\rm mod}(\lambda_i)$ is the model flux density. |
In both cases. the data were fitted by a two-temperature composite model. | In both cases, the data were fitted by a two-temperature composite model. |
It was assumed that both components at different temperatures emit as à blackbody modified by the wavelength-dependent dust opacity. κι (see below). | It was assumed that both components at different temperatures emit as a blackbody modified by the wavelength-dependent dust opacity, $\kappa_{\lambda}$ (see below). |
The best-fit model SEDs overestimate the flux densities at ~12-20 jm. but underestimate them at ~8 and 25 ym. It should be noted that the flux densities included in the SEDs are measured using telescopes with different beam sizes. | The best-fit model SEDs overestimate the flux densities at $\sim12-20$ $\mu$ m, but underestimate them at $\sim8$ and 25 $\mu$ m. It should be noted that the flux densities included in the SEDs are measured using telescopes with different beam sizes. |
Thus the flux densities obtained for extended sources are not fully comparable. and this can in part explain discrepancies between MSX (1873) and IRAS (2' at 12 um to ~4 at 100 jum) fluxes at 12 and ~20—25 yam. On the other hand. SIMBA and LABOCA flux densities at Ξ1.2 mm and 0.87 mm refer to clump areas (Rar is typically ~30") derived byc | Thus the flux densities obtained for extended sources are not fully comparable, and this can in part explain discrepancies between MSX $18\farcs3$ ) and IRAS $\sim2\arcmin$ at 12 $\mu$ m to $\sim4\arcmin$ at 100 $\mu$ m) fluxes at 12 and $\sim20-25$ $\mu$ m. On the other hand, SIMBA and LABOCA flux densities at $\lambda=1.2$ mm and 0.87 mm refer to clump areas $R_{\rm eff}$ is typically $\sim30\arcsec$ ) derived by. |
lumpfind.. Ray values are similar for both [RAS 13037-6122 and IRAS 13039-6108 (~30—40" or ~0.35—0.47 pe). | $R_{\rm eff}$ values are similar for both IRAS 13037-6122 and IRAS 13039-6108 $\sim30-40\arcsec$ or $\sim 0.35-0.47$ pc). |
Assuming that the emission in the IRAS bands is confined in the region of the submm clump. the characteristic spatial scale associated with the SEDs is <0.5 pe. | Assuming that the emission in the IRAS bands is confined in the region of the submm clump, the characteristic spatial scale associated with the SEDs is $\lesssim 0.5$ pc. |
We have adopted a dust-to-gas mass ratio of Ry=1/100. a value which has often been used in the IRDC studies (e.g.. RJSOG: Vasyuninaetal.2009:; Parsonsetal.2009)). | We have adopted a dust-to-gas mass ratio of $R_{\rm d}=1/100$, a value which has often been used in the IRDC studies (e.g., RJS06; \cite{vasyunina2009}; \cite{parsons2009}) ). |
However. this value can differ from 1/100. | However, this value can differ from 1/100. |
For instance. Draine et al. ( | For instance, Draine et al. ( |
2007) determined a value of Ry=1/186 based on observed depletions of heavy elements in the Galaxy. | 2007) determined a value of $R_{\rm d}\approx1/186$ based on observed depletions of heavy elements in the Galaxy. |
Dust opacities we have adopted correspond to a MRN size distribution with thick ice at a gas density of my=10° em (OH94). | Dust opacities we have adopted correspond to a MRN size distribution with thick ice at a gas density of $n_{\rm H}=10^5$ $^{-3}$ (OH94). |
The resulting SED parameters are given in Table 5.. | The resulting SED parameters are given in Table \ref{table:sed}. |
The total (cold+hot) mass and the integrated bolometric luminosity are given in Cols. ( | The total (cold+hot) mass and the integrated bolometric luminosity are given in Cols. ( |
2) and (3) of Table 5.. respectively. | 2) and (3) of Table \ref{table:sed}, respectively. |
The temperatures of the two components are listed in Cols. ( | The temperatures of the two components are listed in Cols. ( |
4) and (5). | 4) and (5). |
In Cols. ( | In Cols. ( |
6) and (7). we give the mass and luminosity fractions of the cold component versus the total mass and luminosity. | 6) and (7), we give the mass and luminosity fractions of the cold component versus the total mass and luminosity. |
Column (8) lists the mass-to-lummosity ratio. Mi/Lpo. Which is an evolutionary indicator of the clump as it is expected to decrease with time. | Column (8) lists the mass-to-luminosity ratio, $M_{\rm tot}/L_{\rm bol}$, which is an evolutionary indicator of the clump as it is expected to decrease with time. |
The envelope mass decreases during the star formation process. and the luminosity of the embedded star or stellar cluster rises (e.g.. Sridharanetal. 2002)). | The envelope mass decreases during the star formation process, and the luminosity of the embedded star or stellar cluster rises (e.g., \cite{sridharan2002}) ). |
We note that the adopted dust opacity model (corresponding to particles coated with thick ice mantles) is not likely to be appropriate for hot dust. and therefore the total bolometric luminosity for the hot component should be taken with caution. | We note that the adopted dust opacity model (corresponding to particles coated with thick ice mantles) is not likely to be appropriate for hot dust, and therefore the total bolometric luminosity for the hot component should be taken with caution. |
The MIR spectral features (such | The MIR spectral features (such |
distribution. | distribution. |
Iu Figure 16.. we show how the Ba» ratio varies for different densitics aud kinetic teniperatures. | In Figure \ref{fig-lvg}, we show how the $_{32}$ ratio varies for different densities and kinetic temperatures. |
It shows that when Ba» varies frou 0.3 to 0.9. the required nunuber deusity of molecular gas changes frou 10? cur? to «10? cu7. | It shows that when $_{32}$ varies from 0.3 to 0.9, the required number density of molecular gas changes from $^{2}$ $^{-3}$ to $\times10^{3}$ $^{-3}$. |
The Rao scems to be dependent on the density more than the temperature when it is below unity. | The $_{32}$ seems to be dependent on the density more than the temperature when it is below unity. |
Tence the variation of Που indicates differcut density among chuups. | Hence the variation of $_{32}$ indicates different density among clumps. |
It is interesting to note that there is a correlation between Ra» aud SFR. aud some chuups (Nl. N2. NT) which have higher SFR values are spatially close to the IICN(J = 10) peaks (soloetal.2003). | It is interesting to note that there is a correlation between $_{32}$ and SFR, and some clumps (N1, N2, N7) which have higher SFR values are spatially close to the HCN(J = 1–0) peaks \citep{koh03}. |
. Wigher values of Ra» will select denser gas associated with higher SER. as has been shown in the large scale observations of ICN and FIR correlation (Gao.Solomon.&Philip200L). | Higher values of $_{32}$ will select denser gas associated with higher SFR, as has been shown in the large scale observations of HCN and FIR correlation \citep{gao04}. |
. In the smaller GAIC-scale. Lada(1992). also showed that the efficiency of star formation is higher iu the dense core rather than in the diffuse eas. | In the smaller GMC-scale, \citet{lada92} also showed that the efficiency of star formation is higher in the dense core rather than in the diffuse gas. |
The ratio map of Ba» can be useful to determine the location of star formation. | The ratio map of $_{32}$ can be useful to determine the location of star formation. |
We thauk the SALA staff for maintaining the operation of the array. | We thank the SMA staff for maintaining the operation of the array. |
We appreciate for referee's detail commuents to iuprove the manuscript. | We appreciate for referee's detail comments to improve the manuscript. |
We thank C. Petitpas for providing the JCAIT data. | We thank G. Petitpas for providing the JCMT data. |
P.-Y. μοι especially acknowledges the fruitful discussious with L.-II. Liu. Ix. Sakamoto. N. Scoville. W. Maciejewski. and L. Πο for the manuscript. | P.-Y. Hsieh especially acknowledges the fruitful discussions with L.-H. Lin, K. Sakamoto, N. Scoville, W. Maciejewski, and L. Ho for the manuscript. |
This project is funded by NSC 97-2112- and NSC 97-2112-M-001-021-MY3. S | This project is funded by NSC 97-2112-M-001-007-MY3 and NSC 97-2112-M-001-021-MY3. , |
This project is funded by NSC 97-2112- and NSC 97-2112-M-001-021-MY3. SM | This project is funded by NSC 97-2112-M-001-007-MY3 and NSC 97-2112-M-001-021-MY3. , |
This project is funded by NSC 97-2112- and NSC 97-2112-M-001-021-MY3. SMA | This project is funded by NSC 97-2112-M-001-007-MY3 and NSC 97-2112-M-001-021-MY3. , |
This project is funded by NSC 97-2112- and NSC 97-2112-M-001-021-MY3. SMA. | This project is funded by NSC 97-2112-M-001-007-MY3 and NSC 97-2112-M-001-021-MY3. , |
This project is funded by NSC 97-2112- and NSC 97-2112-M-001-021-MY3. SMA.. | This project is funded by NSC 97-2112-M-001-007-MY3 and NSC 97-2112-M-001-021-MY3. , |
the filling factor and mass flow constraints (Equations 21 auc 22) must still be valid for any flow in which all or most of the mass flow AL is carried outward by heated regions. | the filling factor and mass flow constraints (Equations 21 and 22) must still be valid for any flow in which all or most of the mass flow ${\dot M}$ is carried outward by heated regions. |
It is likely that our less complicated circulation flows contain essential features that are generic to all ceutrally heated flows desigued to greatlv reduce the cooling rate AT. | It is likely that our less complicated circulation flows contain essential features that are generic to all centrally heated flows designed to greatly reduce the cooling rate ${\dot M}$. |
The idealized circulation flows we describe here could ouly apply for a lanited time because of secular iucrease in the eas mass as new gas enters the circulating region. | The idealized circulation flows we describe here could only apply for a limited time because of secular increase in the gas mass as new gas enters the circulating region. |
For example. if all the eas ejected from evolving red eiaut stars nierees iuto the hot phase. the characteristic time for the hot eas deusity to merease appreciably in NGC 1172 is f.—pfosp.~L2(10kpejtts Cyr where os=LTs1079 tis the current specific rate of stellar mass loss. | For example, if all the gas ejected from evolving red giant stars merges into the hot phase, the characteristic time for the hot gas density to increase appreciably in NGC 4472 is $t_* \sim \rho / \alpha_* \rho_*
\approx 4.2~(r_c/10~{\rm kpc})^{1.18}$ Gyr where $\alpha_* = 4.7 \times 10^{-20}$ $^{-1}$ is the current specific rate of stellar mass loss. |
Moreover. m many galaxv/eroup scale cooling flows. iucludiug NGC. 1172. the hot eas extends far bevoud the circulation radi ο we caleulate here. | Moreover, in many galaxy/group scale cooling flows, including NGC 4472, the hot gas extends far beyond the circulation radii $r_c$ we calculate here. |
Therefore. the cooling iuflow of gas crossing radius vr, provides another secular increase in the mass of gas iu the circulation region. | Therefore, the cooling inflow of gas crossing radius $r_c$ provides another secular increase in the mass of gas in the circulation region. |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.