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{{Sky|11|33|25.4408|-|70|11|41.239|1000000000}}
{{Starbox begin
| name = HD 100546
}}
{{Starbox observe
| epoch = [[J2000.0]]<ref name=SIMBAD/>
| constell = [[Musca]]
| ra = {{RA|11|33|25.4408}}<ref name=SIMBAD>{{Cite web | title = SIMBAD Object query: HD 100546 | url = http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=HD+100546}}</ref>
| dec = {{DEC|-70|11|41.239}}<ref name=SIMBAD/>
| appmag_v = 6.698<ref name=SIMBAD/>
}}
{{Starbox character
| class = B9Vne<ref name=SIMBAD/>
}}
{{Starbox detail
| age = >10<sup>6</sup><ref name=herbig/>
| luminosity =
}}
{{Starbox astrometry
| prop_mo_ra = -38.78<ref name=SIMBAD/>
| prop_mo_dec = -0.05<ref name=SIMBAD/>
| parallax = 9.67<ref name=SIMBAD/>
| p_error = 0.60<ref name=SIMBAD/>
| dist_ly = 337.3<ref name=EPO>{{cite web | title = The Extrasolar Planets Encyclopaedia | url = http://exoplanet.eu/star.php?st=HD+100546}}</ref>
| dist_pc = 103.4<ref name=EPO/>
| absmag_v =
}}
{{Starbox catalog
| names = V* KR Mus, SAO 251457, CD-69 893, [[Hipparcos catalogue|HIP]] 56379, [[Henry Draper catalogue|HD]] 100546.<ref name=SIMBAD/>
}}
{{Starbox end}}


{{Planetbox begin
[[Image:SodShockTubeTest Regions.png|thumb|300px|right|Density Plot after time evolution of t=0.2[-]]]
| name = HD 100546 B
The '''Sod shock tube''' problem, named after Gary A. Sod, is a common test for the accuracy of [[Computational fluid dynamics|computational fluid codes]], like [[Riemann solver]]s, and was heavily investigated by Sod in 1978.
}}|  
{{Planetbox star
| star = HD 100546
| RA =   {{RA|11|33|25.4408}}<ref name=SIMBAD/>
| DEC = {{DEC|-70|11|41.239}}<ref name=SIMBAD/>
| class = B9Vne<ref name=SIMBAD/>
}}
{{Planetbox character
| mass = ~20<ref name=planet-1/>
}}
{{Planetbox orbit
| semimajor = 6.5<ref name=planet-1/>
}}
{{Planetbox end}}


'''HD 100546''' is a star 337.3 [[Light year|LY]] from [[Earth]]. It is orbited by an approximately 20 [[Jupiter|M<sub>j</sub>]] [[planet]] at 6.5 [[Astronomical unit|AU]].<ref name=planet-1>{{Cite journal | title = Resolving the disk rotation of HD 97048 and HD 100546 in the <nowiki>[O I]</nowiki> 6300A line: evidence for a giant planet orbiting HD 100546 | last = Acke | first = B. | coauthors = van der Ancker; M. | journal = Astronomy and Astrophysics | date = November 2005 | volume = 449 | issue = 267 | arxiv = astro-ph/0512562|doi = 10.1051/0004-6361:20054330 | bibcode=2006A&A...449..267A | pages = 267}}</ref>
The test consists of a one-dimensional [[Riemann problem]] with the following parameters, for left and right states of an [[ideal gas]].


==HD 100546 B==
<center>
Evidence for a planetary companion to HD 100546 was gathered using the UVES [[Echelle grating|echelle spectrograph]] at the [[Very Large Telescope|VLT]] in [[Chile]].<ref name=planet-1/> This confirms other data indicating a planetary companion.  The planet's size puts it near the border between a giant planet and a [[brown dwarf]].<ref name=planet-1/>
<math>
\left( \begin{array}{c}\rho_L\\P_L\\v_L\end{array}\right)
=
\left( \begin{array}{c}1.0\\1.0\\0.0\end{array} \right)
</math>
,
<math>
\left( \begin{array}{c}\rho_R\\P_R\\v_R\end{array}\right)
=
\left( \begin{array}{c}0.125\\0.1\\0.0\end{array}\right)
</math>
</center>
where
::*<math>\rho</math> is the density
::*P  is the pressure
::*v is the velocity


==Protoplanetary material==
The time evolution of this problem can be described by solving the [[Euler equations]].
Spectroscopic analysis of mid-IR data taken from OSCIR on the 4 m [[Victor M. Blanco Telescope|Blanco Telescope]] at [[Cerro Tololo Inter-American Observatory]] indicates the presence of a small particles (10 - 18 <math>\mu  m</math>) containing [[silicates]].<ref name=herbig>{{Cite journal | title = The Disk and Environment of the Herbig Be Star HD 100546 | first = C. A. | last = Grady | date = December 2001 | journal = The Astronomical Journal | volume = 122 | issue = 6 | pages = 3396–3406 | doi = 10.1086/324447 | url = http://www.iop.org/EJ/article/1538-3881/122/6/3396/201085.html | last2 = Polomski | first2 = E. F. | last3 = Henning | first3 = Th. | last4 = Stecklum | first4 = B. | last5 = Woodgate | first5 = B. E. | last6 = Telesco | first6 = C. M. | last7 = Piña | first7 = R. K. | last8 = Gull | first8 = T. R. | last9 = Boggess | first9 = A. | bibcode=2001AJ....122.3396G}}</ref>  The material is found at distances out to 17 [[Astronomical unit|AU]] away from the star and has a temperature of approximately 227 [[Kelvin|K]].<ref name=herbig/>
Which leads to three characteristics, describing the propagation speed of the
various regions of the system. Namely the rarefaction wave, the contact discontinuity and
the shock discontinuity.
If this is solved numerically, one can test against the analytical solution,
and get information how well a code captures and resolves shocks and contact discontinuities
and reproduce the correct density profile of the rarefaction wave.


==References==
==Analytic derivation==
{{Reflist}}
The different states of the solution are separated by the time evolution of the
three [[Method of characteristics|characteristics]] of the system, which is due to the finite speed
of information propagation. Two of them are equal to the speed
of sound of the both states
::<math>cs_1 = \sqrt{\gamma \frac{P_L}{\rho_L}}</math>
::<math>cs_5 = \sqrt{\gamma \frac{P_R}{\rho_R}}</math>
The first one is the position of the beginning of the rarefaction wave while
the other is the velocity of the propagation of the shock.


==Further reading==
Defining:
*{{Cite journal | title = Catalog of Nearby Exoplanets | last = Butler | first = P. | coauthors = Wright, J.; Marcy, G.; Fischer, D.; Vogt, S.; Tinney, Ch.; Jones, H.; Carter, B.; Penny, A | journal = The Astrophysical Journal | volume = 646 | issue = 505 | pages = 505–522 | date = March 2006 | arxiv = astro-ph/0607493 | doi = 10.1086/504701 | bibcode=2006ApJ...646..505B}}
::<math>\Gamma = \frac{\gamma - 1}{\gamma + 1}</math>, <math>\beta = \frac{\gamma - 1}{2 \gamma}</math>
 
The states after the shock are connected by the [[Rankine-Hugoniot equation|Rankine Hugoniot]]
*{{Cite journal | title = Kinematics of planet-host stars and their relation to dynamical streams in the solar neighbourhood | last = Ecuvillon | first = A. | coauthors = Israelian, G.; Pont, F.; Santos, N.; Mayor, M. | journal = Astronomy and Astrophysics | date = August 2006 | volume = 461 | issue = 171 | arxiv = astro-ph/0608669|doi = 10.1051/0004-6361:20065872 | pages = 171–182 | bibcode=2007A&A...461..171E}}
shock jump conditions.
 
::<math>\rho_4 = \rho_5 \frac{P_4 + \Gamma P_5}{P_5 + \Gamma P_4}</math>
*{{Cite journal | title = Habitability of known exoplanetary systems based on measured stellar properties | last = Jones | first = B. | coauthors = Sleep, P.; Underwood, D. | journal = The Astrophysical Journal | date = June 2006 | volume = 649 | issue = 1010 | arxiv = astro-ph/0603200|bibcode = 2006ApJ...649.1010J |doi = 10.1086/506557 | pages = 1010–1019 }}
But to calculate the density in Region 4 we need to know the pressure in that region.
 
This is related by the contact discontinuity with the pressure in region 3 by
*{{Cite journal | title = Formation of Earth-like Planets During and After Giant Planet Migration | last = Mandell, A.; Raymond, S.; Sigurdsson, S | date = | journal = The Astrophysical Journal | volume = 660 | issue =  | arxiv = astro-ph/0701048 |bibcode =  2007ApJ...660..823M|doi = 10.1086/512759 | first1 = Avi M. | last2 = Raymond | first2 = Sean N. | last3 = Sigurdsson | first3 = Steinn | pages = 823–844 }}
::<math>P_4 = P_3</math>
 
Unfortunately the pressure in region 3 can only be calculated iteratively, the right
*{{Cite journal | title = Extrasolar planet taxonomy: a new statistical approach | last = Marchi | first = S. | date = May 2007 | journal = The Astrophysical Journal | volume = 666 | issue =  | arxiv = 0705.0910|bibcode = 2007ApJ...666..475M |doi = 10.1086/519760 | pages = 475–485 }}
solution is found when <math>u_2</math> equals <math>u_4</math>
 
::<math>u_4 = \left(P_3' - P_5\right)\sqrt{\frac{1-\Gamma}{\rho_R(P_3'+\Gamma P_5)}}</math>
*{{Cite journal | title = The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs | last = Nortdstrom, R.; Mayor, M.; Andersen, J.; Holmberg, J; Pont, F.; Jorgenson, B.; Olsen, E.; Udry, S.; Mowlavi, N | journal = Astronomy and Astrophysics | volume = 418 | issue = 989 | arxiv = astro-ph/0405198|bibcode = 2004A&A...418..989N |doi = 10.1051/0004-6361:20035959 | year = 2004  | pages = 989–1019 | first1 = B. | last2 = Mayor | first2 = M. | last3 = Andersen | first3 = J. | last4 = Holmberg | first4 = J. | last5 = Pont | first5 = F. | last6 = j�Rgensen | first6 = B. R. | last7 = Olsen | first7 = E. H. | last8 = Udry | first8 = S. | last9 = Mowlavi | first9 = N. }}
::<math>u_2 =\left(P_1^\beta-P_3'^\beta\right) \sqrt{\frac{(1-\Gamma^2)P_1^{1/\gamma}}{\Gamma^2 \rho_L}}</math>
 
::<math>u_2 - u_4 = 0</math>
*{{Cite journal | title = The Circumstellar Dust Disk of HD 100546 | last = Hedrick | first = C. H. | coauthors =  Doering, R.; Lee,  K.-G.; Sosey, M.; Meixner, M.; Ardila, D. | journal = American Astronomical Society | date = January 2006 | volume = 37 | issue = 4 | url = http://www.aas.org/publications/baas/v37n4/aas207/1013.htm}}
This function can be evaluated to an arbitrary precision thus giving the pressure in the
 
region 3
==External links==
::<math>P_3 = \operatorname{calculate}(P_3,s,s,,)</math>
*[http://zuserver2.star.ucl.ac.uk/~apod/apod/ap010502.html Astronomy picture of the day] - May 2, 2001
finally we can calculate
 
::<math>u_3 = u_5 + \frac{(P_3 - P_5)}{\sqrt{\frac{\rho_5}{2}((\gamma+1)P_3 +(\gamma-1)P_5)}}</math>
[[Category:Extrasolar planets]]
::<math>u_4 = u_3</math>
and <math>\rho_3</math> follows from the adiabatic gas law
::<math>\rho_3 = \rho_1 \left(\frac{P_3}{P_1}\right)^{1/\gamma}</math>


==References==
*{{cite journal | title=A Survey of Several Finite Difference Methods for Systems of Nonlinear Hyperbolic Conservation  Laws | first=G. A. | last=Sod | year=1978 | journal=[[Journal of Computational Physics|J. Comput. Phys.]] | volume=27| pages=1–31 | url=http://www.osti.gov/energycitations/product.biblio.jsp?osti_id=6812922 | doi=10.1016/0021-9991(78)90023-2 |bibcode = 1978JCoPh..27....1S }}
*{{cite book | first=Eleuterio F.| last=Toro| year=1999 | title=Riemann Solvers and Numerical Methods for Fluid Dynamics| publisher=Springer Verlag|location=Berlin | id=ISBN 3-540-65966-8}}


{{star-stub}}
==See also==
{{extrasolar-planet-stub}}
*[[Shock tube]]
*[[Computational fluid dynamics]]


[[fa:اچ‌دی ۱۰۰۵۴۶]]
[[Category:Fluid dynamics]]
[[ru:HD 100546]]
[[Category:Computational fluid dynamics]]

Revision as of 13:46, 16 August 2014

Density Plot after time evolution of t=0.2[-]

The Sod shock tube problem, named after Gary A. Sod, is a common test for the accuracy of computational fluid codes, like Riemann solvers, and was heavily investigated by Sod in 1978.

The test consists of a one-dimensional Riemann problem with the following parameters, for left and right states of an ideal gas.

,

where

The time evolution of this problem can be described by solving the Euler equations. Which leads to three characteristics, describing the propagation speed of the various regions of the system. Namely the rarefaction wave, the contact discontinuity and the shock discontinuity. If this is solved numerically, one can test against the analytical solution, and get information how well a code captures and resolves shocks and contact discontinuities and reproduce the correct density profile of the rarefaction wave.

Analytic derivation

The different states of the solution are separated by the time evolution of the three characteristics of the system, which is due to the finite speed of information propagation. Two of them are equal to the speed of sound of the both states

The first one is the position of the beginning of the rarefaction wave while the other is the velocity of the propagation of the shock.

Defining:

,

The states after the shock are connected by the Rankine Hugoniot shock jump conditions.

But to calculate the density in Region 4 we need to know the pressure in that region. This is related by the contact discontinuity with the pressure in region 3 by

Unfortunately the pressure in region 3 can only be calculated iteratively, the right solution is found when equals

This function can be evaluated to an arbitrary precision thus giving the pressure in the region 3

finally we can calculate

and follows from the adiabatic gas law

References

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See also