# 1997A&A...327....1F

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 Query : 1997A&A...327....1F

1997A&A...327....1F - Astronomy and Astrophysics, volume 327, 1-7 (1997/11-1)

Magnetic fields and large-scale structure in a hot universe. II. Magnetic flux tubes and filamentary structure.

FLORIDO E. and BATTANER E.

Abstract (from CDS):

In Paper I, we obtained an equation for the evolution of density inhomogeneities in a radiation dominated universe when they are affected by magnetic fields. In this second paper we apply this equation to the case in which the subjacent magnetic configuration is a flux tube. For scales of the order of 1Mpc or less the differential equation is elliptical. To solve it, we have used the numerical method based on Simultaneous Over Relaxation", SOR, with Chebyshev acceleration and we have treated the problem as a boundary value problem, which restricts the prediction ability of the integration. For large-scale flux tubes, much larger than 1Mpc, the equation can be analytically integrated and no assumption about the final shape or magnitude of the inhomogeneity is required. In both cases we obtain an evolution which does not differ very much from linear in time. The inhomogeneity in the density becomes filamentary. Large scale structures (≥10Mpc) are probably unaffected by damping, non-linear and amplification mechanisms after Equality, so that this model provides a tool to interpret the present observed large scale structure. Filaments are very frequently found in the large-scale structure in the Universe. It is suggested here that they could arise from primordial magnetic flux tubes, thus providing an alternative hypothesis for its interpretation; in particular we consider the case of the Coma-A1367 supercluster, where the magnetic field is known to be high.

Journal keyword(s): magnetohydrodynamics - relativity - cosmology: large-scale structure of Universe

 Number of rows : 1
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1036 1

 Query : 1997A&A...327....1F

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', {sourceSize:12, color:'#30a090'})); aladin.on('objectClicked', function(object) { var objName=object.data.MAIN_ID; aladin.showPopup(object.ra,object.dec,'',''+ objName+''); });" title="Show Simbad objects"> Overlay points in this preview
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 Some important notes on this object about identifications and objects associations. notes: Brightest Galaxy of the cluster is NGC 3842 (Hudson et al., 2001MNRAS.327..265H)

Hierarchy : number of linked objects
whatever the membership probability is (see description here ) :

 The count displayed here is the number of children objects. The list obtained by clicking the button may be larger, as some children may be linked with different references or probability. %This number is the number of distinct objets linked, by using this button, you will obtain all links (may be more than one) from that object to his children : 579 Display criteria : All >=90% stars galaxies radio IR <2 arcsec #ref>50

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 ACO 1367 HMS 1142+2035 RASSCALS NRGb155 WBL 353 2A 1141+199 INTREF 460 RBS 1026 XSS J11444+1952 3A 1141+198 1M 1144+197 RXC J1144.7+1949 [F81] 215 BAX 176.1231+19.8391 2MAXI J1144+198 RXC J1144.6+1945 [N93] 78 ClG 1141.9+2007 MCXC J1144.6+1945 1RXS J114452.7+194706 [S85] 131 1E 1141.9+2007 PLCKESZ G234.59+73.01 2U 1144+19 [SPD2011] 227 FR 70 PSZ1 G234.54+73.03 3U 1144+19 1H 1142+199 PSZ2 G234.59+73.01 4U 1143+19

 References (1036 between 1850 and 2022) (Total 1036) Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system). Follow new references on this object
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 ACO 1367 RXC J1144.7+1949 RXC J1144.6+1945 1RXS J114452.7+194706

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2022.05.28-07:02:14