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Ouce again. while te known correation in O/H versus L is clea‘ly Sowl. the correlatio ris much weaker (or absen) for Ο/Η versis surface brielituess. | Once again, while the known correlation in O/H versus L is clearly shown, the correlation is much weaker (or absent) for O/H versus surface brightness. |
I would aopea‘that this comparative study stpports luminosity as the imporalt paraineter. | It would appear that this comparative study supports luminosity as the important parameter. |
]t would |ye Dest o place this σοιclusion on a firijer statistical base. bu the samgle size is sinall ancl Wontnifom. | It would be best to place this conclusion on a firmer statistical base, but the sample size is small and non-uniform. |
In ¢uder to invetigze only the scaer in Figure 5. we lave assumed errors of 0.1 dex in all of the abutdance measurenents and 0.2 1ag in the Iumninosities and surface brightness. | In order to invetigate only the scatter in Figure 8, we have assumed errors of 0.1 dex in all of the abundance measurements and 0.2 mag in the luminosities and surface brightness. |
Then performing a litlear least squares fit to both saiiples yields nearly identical vaues of u (60). even though tlie samdle with Iumiuosities is larger 19 versus 13). | Then performing a linear least squares fit to both samples yields nearly identical values of $\chi ^2$ (60), even though the sample with luminosities is larger (19 versus 13). |
Ruwing the saije test on only the galaxies with bot1 luminosities aud surface brightnesses vields a [αςor of two lewer V? lor the regression against luiiinosity (coulirmine what tlie eve sees in Figure 5. | Running the same test on only the galaxies with both luminosities and surface brightnesses yields a factor of two lower $\chi ^2$ for the regression against luminosity (confirming what the eye sees in Figure 8). |
We repea that it would be best to perform {1is type of test with a larger database with uniform error estimates. | We repeat that it would be best to perform this type of test with a larger database with uniform error estimates. |
There has been a long staudiug debate coucerning the role of galactic winds in the evolution ol dwarf galaxies (see Skillman LOOT [or a review). | There has been a long standing debate concerning the role of galactic winds in the evolution of dwarf galaxies (see Skillman 1997 for a review). |
Oue aspect of this debate coucerus the yields derived from the observations of dwarf galaxies. | One aspect of this debate concerns the yields derived from the observations of dwarf galaxies. |
Often. the calculated yields are signilicautly lower than theoretically expected vields. aud this has been taken as good evidence of losses clue to metal enriched winds (Matteucci Chiosi 1983). | Often, the calculated yields are significantly lower than theoretically expected yields, and this has been taken as good evidence of losses due to metal enriched winds (Matteucci Chiosi 1983). |
Iu the simple closed box mocel with instantaneous recycling (Searle Sargeut 1972). the gas phase abundance (Z) is related directly to the baryonie gas mass fraction (yr) as: | In the simple closed box model with instantaneous recycling (Searle Sargent 1972), the gas phase abundance $Z$ ) is related directly to the baryonic gas mass fraction $\mu$ ) as: |
expert help tended by the ISRO specialists. | expert help tended by the ISRO specialists. |
The latter helped significantly in debugeing the various problems that appeared during the integration. | The latter helped significantly in debugging the various problems that appeared during the integration. |
A full eud-to-end. test of TAUVEN and GSAT-1 was performed at the completion of the integration. | A full end-to-end test of TAUVEX and GSAT-4 was performed at the completion of the integration. |
This incuded moving the MDP to prese angles and nieasurine the LOS, acquiring diffuse light images and sending them to the EGSE through the GSAT-1l telemetry system, ete; | This included moving the MDP to preset angles and measuring the LOS, acquiring diffuse light images and sending them to the EGSE through the GSAT-4 telemetry system, etc. |
All these functioued perfectly. except that whenever GSAT-1 was operated from the solar panel simulator instead of a UPS strange patterus appeare in the TAUVEN images and the point spread πιοος of uiresolved. pinhole sources became excessively large. | All these functioned perfectly, except that whenever GSAT-4 was operated from the solar panel simulator instead of a UPS strange patterns appeared in the TAUVEX images and the point spread functions of unresolved pinhole sources became excessively large. |
It was clear that we had a noise pickup problem in the TAUVEX power supply: this was fixed by adding a filtering stage to the TAUVEN power input at the GSAT-1 end. | It was clear that we had a noise pickup problem in the TAUVEX power supply; this was fixed by adding a filtering stage to the TAUVEX power input at the GSAT-4 end. |
It is worth stressing that at the end of the αι intceration not only was TÀUVEX itself ready for launch. but also the science teams were ready for the mission in software, nission planning and science planning. | It is worth stressing that at the end of the final integration not only was TAUVEX itself ready for launch, but also the science teams were ready for the mission in software, mission planning and science planning. |
In particular, exercises of the two teas were held to prove the reduction pipeline, including the reconstruction of the UW images collected by the three telescopes using artificial event streams as well as real data collected durug the ground. calibrations. | In particular, exercises of the two teams were held to prove the reduction pipeline, including the reconstruction of the UV images collected by the three telescopes using artificial event streams as well as real data collected during the ground calibrations. |
A detailed iission plan for the first flight mouths was also generated: it included the space acceptance tests discussed above in ον | A detailed mission plan for the first flight months was also generated; it included the space acceptance tests discussed above in \ref{qual}. |
Since spring 2009 rumors beean to filter to the TAUVENBS cain about possible problems with the GSAT- linissiou | Since spring 2009 rumors began to filter to the TAUVEX team about possible problems with the GSAT-4 mission. |
These were never more than word-of-mouth statements waving to do with uncertainties regarding the capahbilitics§f of the lanucher. | These were never more than word-of-mouth statements having to do with uncertainties regarding the capabilities of the launcher. |
Nevertheless. at the completion of the final pre-launch integration stage, performed to the satisfaction of both ISRO aud El-Op teams. the ELOp eneineers and the TAUVEX scientists were convinced hat only a few more steps had to be completed in the rear future before starting to enjov the scientific output roni TAUVEN: a final vibration and acoustic noise est of the complete satellite including TAUVEX, and a partial test of TAUVEN with GSAT-1 at the launch site. prior to the satellite integration with the GSLV vehicle. | Nevertheless, at the completion of the final pre-launch integration stage, performed to the satisfaction of both ISRO and El-Op teams, the El-Op engineers and the TAUVEX scientists were convinced that only a few more steps had to be completed in the near future before starting to enjoy the scientific output from TAUVEX: a final vibration and acoustic noise test of the complete satellite including TAUVEX, and a partial test of TAUVEX with GSAT-4 at the launch site, prior to the satellite integration with the GSLV vehicle. |
The ΒΙΟ was supposed to follow promptly in January or February 2010. | The launch was supposed to follow promptly in January or February 2010. |
In December 2009. ISRO officials contacted the TAUVEN tea and suggested that it might be advisable to take TAUVEN off the satellite because of concerus that he satellite iiass was too high to allow a lifetime longer than 6 months in orbit. | In December 2009, ISRO officials contacted the TAUVEX team and suggested that it might be advisable to take TAUVEX off the satellite because of concerns that the satellite mass was too high to allow a lifetime longer than 6 months in orbit. |
In addition, there were sugeestious based on an earlier GSAT fight that lelt scattered by the GSAT-1 solar panels would adversely affect observations toward the celestial poles; where 1ο best TAUVEN data would have come from. | In addition, there were suggestions based on an earlier GSAT flight that light scattered by the GSAT-4 solar panels would adversely affect observations toward the celestial poles, where the best TAUVEX data would have come from. |
The TAUVEN team was not able to independently quantify us additional contribution to the scattered lieht. | The TAUVEX team was not able to independently quantify this additional contribution to the scattered light. |
During these discussions with the ISRO officiaρα rey mentioned a possibility to launch TAUVEN ou sinall dedicated satellite that could be lofted to ow Earth orbit with a PSLV launch. | During these discussions with the ISRO officials, they mentioned a possibility to launch TAUVEX on a small dedicated satellite that could be lofted to low Earth orbit with a PSLV launch. |
This option. lat appeared to the science teams to be senuinc. would essentially have restored TAUVEX to its original nission as proposed to ISA and described in ??.. | This option, that appeared to the science teams to be genuine, would essentially have restored TAUVEX to its original mission as proposed to ISA and described in \ref{intro}. |
Although neither ISA nor Tel Aviv University or Op ever agreed to the removal of TAUVEN from GSAT- bv late-Januuary or carly-February 2010 the A\IDP with TAUVEN were unloaded from GSAT-1 aud. the satellite was closed wp for launch. | Although neither ISA nor Tel Aviv University or El-Op ever agreed to the removal of TAUVEX from GSAT-4, by late-January or early-February 2010 the MDP with TAUVEX were unloaded from GSAT-4 and the satellite was closed up for launch. |
TAUVEN was left in the ISRO clean room. protected by clean anti-static plastic sheets. | TAUVEX was left in the ISRO clean room, protected by clean anti-static plastic sheets. |
ISRO. decided to launch GSEV. carrvinge GSAT-1 on 15 April 2010 despite the possibility that the crvogcuic upper stage ofthe launcher would not fiction properly. | ISRO decided to launch GSLV carrying GSAT-4 on 15 April 2010 despite the possibility that the cryogenic upper stage of the launcher would not function properly. |
The launch was broadcast live and the Israeli team viewed it in real time. | The launch was broadcast live and the Israeli team viewed it in real time. |
About 500- seconds following ignition, after the first and second stages completed heir burning. the third (crvogenic) upper stage lit up but apparently could not sustain the burn. | About 500 seconds following ignition, after the first and second stages completed their burning, the third (cryogenic) upper stage lit up but apparently could not sustain the burn. |
The rocket was seen not accelerating. taking a nose dip. osing attitude control. and prestunably crashing iuto he ocean. | The rocket was seen not accelerating, taking a nose dip, losing attitude control, and presumably crashing into the ocean. |
The TAUVEN team expericuced mixed feelines. | The TAUVEX team experienced mixed feelings. |
Ou he one hand they grieved for the loss of the satellite id launcher. and for the waste of so mam, vears [hard work bv the dedicated ISRO teams. | On the one hand they grieved for the loss of the satellite and launcher, and for the waste of so many years of hard work by the dedicated ISRO teams. |
Ou the other hand. they felt an obvious sense of relief that TAUVEN was spared. remaining safe in the ISRO CiCali TOOL. and expecting to fly on a future platform. | On the other hand, they felt an obvious sense of relief that TAUVEX was spared, remaining safe in the ISRO clean room, and expecting to fly on a future platform. |
However. up to the time this paper was written. the inter-ageney contacts did uot vet vield a date or a specific platform that could loft TAUVEN to perform its intended scicutific tasks. | However, up to the time this paper was written, the inter-agency contacts did not yet yield a date or a specific platform that could loft TAUVEX to perform its intended scientific tasks. |
In the meantime. TAUVEN was dismounted from the MDP by an ELOp eani and was securely stored m its transportation container that provides an optimal storage environnient since it is filled with dry nitrogen. | In the meantime, TAUVEX was dismounted from the MDP by an El-Op team and was securely stored in its transportation container that provides an optimal storage environment since it is filled with dry nitrogen. |
The container with TAUVEX is storec in the ISRO clean yoo in Bangalore. | The container with TAUVEX is stored in the ISRO clean room in Bangalore. |
Given the delay till a possible launch would become available. it became clear to the science teams of both | Given the delay till a possible launch would become available, it became clear to the science teams of both |
The basic equatious governing plasma outflows iu the framework of an ideal ΑΠΟ treatineut for steady. ο flows are the ΠοΕΕ mass aud magnetic flux conservation. the frozen-in law for infinite conductivitv. and the first law of thoerinodyuauies. | The basic equations governing plasma outflows in the framework of an ideal MHD treatment for steady, axisymmetric flows are the momentum, mass and magnetic flux conservation, the frozen-in law for infinite conductivity, and the first law of thermodynamics. |
Iu particular. the poloidal component of the magnetic field can be derived from the imagnetie flux im spherical coordinates Gr.0. V7). We need to specify the latidudinal dependences of the velocity. iiagnoetic. density aud pressure fields. V. B. P and p respectively, | In particular, the poloidal component of the magnetic field can be derived from the magnetic flux in spherical coordinates $r, \theta, \varphi$ ), We need to specify the latidudinal dependences of the velocity, magnetic, density and pressure fields, $\vec{V}$ , $\vec{B}$, $P$ and $\rho$ respectively. |
This can be resumed in the following assuniptious (for details sce ST91. STT99 and STT02): Weused (Πο)&Ποσο. 1976)) | This can be resumed in the following assumptions (for details see ST94, STT99 and STT02): Weused \citeauthor{KoppHolzer76}, \citeyear{KoppHolzer76}) |
This can be resumed in the following assuniptious (for details sce ST91. STT99 and STT02): Weused (Πο)&Ποσο. 1976)): | This can be resumed in the following assumptions (for details see ST94, STT99 and STT02): Weused \citeauthor{KoppHolzer76}, \citeyear{KoppHolzer76}) |
Perhaps the most important kinematic property of disk galaxies is their. angular momentum. as this quantity determines the sizes of thin. rotationally supported disks (Moetal. 1998).. | Perhaps the most important kinematic property of disk galaxies is their angular momentum, as this quantity determines the sizes of thin, rotationally supported disks \citep{mmw98a}. |
"ncWhile measuring: the specificMN angular momentum j. of each star particle is straightforward. deciding which particles to use for measuring the angular momentum content theN disk is .less clear. in particular: when. comparing with: where observations. | While measuring the specific angular momentum $j_{\star}$ of each star particle is straightforward, deciding which particles to use for measuring the angular momentum content of the disk is less clear, in particular when comparing with observations. |
. We; wish. to compare our simulated. galaxy with. the /- relation: measured= byMathewson etal.=pand↙↴⊀ Courteau "(1997)andSO the corresponding .j.—⋅ Vo∩∙↭−↓⊃∣∖∶↭↑⋯∶↔⊺≏↧∣≏↧⇀∖⋝∁∣⊽ (as compiledbyNavarro1998). | We wish to compare our simulated galaxy with the $I$ -band Tully-Fisher relation measuredby \cite{mfb92a} and \cite{courteau97a} and the corresponding $j_{\star}-V_{\mathrm{rot}}$ relation \citep[as compiled
by][]{navarro98a}. |
.The measured rotation velocity V, used for these relations is determined observationally at 2.2 times the exponential scale-length of the stellar surface: brightness.: S Ry. | The measured rotation velocity $V_{\rm rot}$ used for these relations is determined observationally at $2.2$ times the exponential scale-length of the stellar surface brightness, $R_{d}$ . |
Weuw then take V4,: to be Αρ is the B-band surface brightness scale-length of determined in 4.2.. | We then take $V_{\rm rot}$ to be where $R_{d,B}$ is the $B$ -band surface brightness scale-length determined in \ref{subsec:phot}. |
In what follows. when we refer to V4, we always⇁⇁ mean the expected- rotation⊀↼ velocity; ↼⇁↤corresponding; to circular velocityLl. uuproduced ↼⇁⊲by all. mass within 2.2ee « gs (1992)t | In what follows, when we refer to $V_{\rm rot}$ we always mean the expected rotation velocity corresponding to the circular velocity produced by all mass within $2.2 \times R_{d,B}=0.045 R_{200}$ for galaxy C1. |
Having determmed the rotation velocity Vij. we then consider 3 different approaches for measuring the specific | Having determined the rotation velocity$V_{\rm rot}$ , we then consider 3 different approaches for measuring the specific |
perfect. especially in the transition between the linear and non-linear reginie. | perfect, especially in the transition between the linear and non-linear regime. |
The total power spectrum is the sum of the two contributions. P(À)DOqPPky. | The total power spectrum is the sum of the two contributions, $P(k)=P^{hh}(k)+P^P(k)$. |
On small scales. the Poisson term dominates. | On small scales, the Poisson term dominates. |
On larger scales. the halo-halo term dominates and reduces to the linear power spectrum. | On larger scales, the halo-halo term dominates and reduces to the linear power spectrum. |
From here forward. we express the power spectrum in dimensionless form. (&)=AslP). | From here forward, we express the power spectrum in dimensionless form, $\Delta^2(k)=4\pi k^3 P(k)$. |
The elfect on the power spectrum of varving ej and 3 in à tvpical ACDAL cosmology is shown in Figure L.. | The effect on the power spectrum of varying $c_0$ and $\beta$ in a typical $\Lambda$ CDM cosmology is shown in Figure \ref{fig:varyc0beta}. |
The concentration controls how tightly matter is correlated.| within a single. halo. | The concentration controls how tightly matter is correlated within a single halo. |
Therefore. higher concentration means a larger one-halo term. | Therefore, higher concentration means a larger one-halo term. |
Increasing. co increases the concentration at the non-linear mass. allecting the amplitude of the power spectrum where it is dominated bv onc-halo term. | Increasing $c_0$ increases the concentration at the non-linear mass, affecting the amplitude of the power spectrum where it is dominated by one-halo term. |
Varving 3 keeping ον constant produces a tilt in the non-linear power spectrum around the fiducial value. which is set by the scale where the non-linear mass dominates the power spectrum contribution (k30 40 4 Alpe +). | Varying $\beta$ keeping $c_0$ constant produces a tilt in the non-linear power spectrum around the fiducial value, which is set by the scale where the non-linear mass dominates the power spectrum contribution $k \sim 30$ $40$ $h$ $^{-1}$ ). |
Haloes less massive than the non-linear mass dominate at higher &. | Haloes less massive than the non-linear mass dominate at higher $k$. |
Steeper (more negative) 2 means that haloes less massive than the non-linear mass willhave their concentrations enhanced. leacing to an enhanced one-halo term. and more power at high A. | Steeper (more negative) $\beta$ means that haloes less massive than the non-linear mass willhave their concentrations enhanced, leading to an enhanced one-halo term, and more power at high $k$. |
Haloes more massive than the non-linear mass will have their concentration reduced. | Haloes more massive than the non-linear mass will have their concentration reduced. |
These dominate at intermediate A in the non-linear regime. so power there is reduced. | These dominate at intermediate $k$ in the non-linear regime, so power there is reduced. |
The changes in 2 shown in the figure may. not have much effect. on the power spectrum at &<100 f +. which is the range where N-body simulations are reliable. | The changes in $\beta$ shown in the figure may not have much effect on the power spectrum at $k<100$ $h$ $^{-1}$, which is the range where $N$ -body simulations are reliable. |
On the other hand. they have a substantial effect on the concentration of twpical-sizect haloes. | On the other hand, they have a substantial effect on the concentration of typical-sized haloes. |
For the same concentration. at the non-lincar. mass (~10713/>tALL). a halo at 107712 fh1 AM. has a concentration. lower with §=Ql than with 7=O04. | For the same concentration at the non-linear mass $\sim 10^{13}\ h^{-1}\ M_{\sun}$ ), a halo at $10^{12}$ $h^{-1}$ $M_{\sun}$ has a concentration lower with $\beta=-0.1$ than with $\beta=-0.4$. |
These masses do not dominate the power spectrum until &>100 5 1. κο this change does not make as much of a dillerence on the power spectrum at scales larger than this. | These masses do not dominate the power spectrum until $k>100$ $h$ $^{-1}$, so this change does not make as much of a difference on the power spectrum at scales larger than this. |
This cliseussion sugeests that while power spectrum analysis cannot provide strong Constraints on the mass dependence of concentration. one can use concentration mass relation to predict. the power spectrum at small scales which are not resolved. by simulations. | This discussion suggests that while power spectrum analysis cannot provide strong constraints on the mass dependence of concentration, one can use concentration mass relation to predict the power spectrum at small scales which are not resolved by simulations. |
Weconsider two sets of cases which have been extensively simulated. self-similar initial conditions ancl more realistic cold dark matter initial conditions. | Weconsider two sets of cases which have been extensively simulated, self-similar initial conditions and more realistic cold dark matter initial conditions. |
In both cases we use the fitting formulae for non-linear 27(&) given by ?.. | In both cases we use the fitting formulae for non-linear $\Delta^2(k)$ given by \citet{2002astro.ph..7664S}. |
The simplest case to consider is Q=1 Einstein-de Sitter universe with a power law linear power spectrum. | The simplest case to consider is $\Omega=1$ Einstein-de Sitter universe with a power law linear power spectrum. |
In this case. 3 has an analytic form. provicled we assumethat once a halo collapses. the scale radius rs is fixed in. proper coordinates. | In this case, $\beta$ has an analytic form, provided we assumethat once a halo collapses, the scale radius $r_s$ is fixed in proper coordinates. |
Ες is suggested by the simple model which assumes the haloes remain unchanged once formed. which seems to hold in numerical simulations (2).. | This is suggested by the simple model which assumes the haloes remain unchanged once formed, which seems to hold in numerical simulations \citep{2001MNRAS.321..559B}. . |
We follow the evolution of a singlehalo. as it traces out a portion of the CCAL) relation. | We follow the evolution of a singlehalo, as it traces out a portion of the $c(M)$ relation. |
1n an O=I universe. density perturbations grow as the scale factor a=1/(1|). | In an $\Omega=1$ universe, density perturbations grow as the scale factor $a=1/(1+z)$. |
For a power law linear spectrum. this. means Pui(&)xDphsoack’. | For a power law linear spectrum, this means $P_{\rm lin}(k) \propto a^2 k^n$. |
cpTop-hat smoothing. at the scale corresponding to AL vieldse(AM)xaM9 . | Top-hat smoothing at the scale corresponding to $M$ yields $\sigma(M) \propto a M^{-{n+3 \over 6}}$. |
Foran£,,—1 universe. ὃς&1.68 is constant in time. so a(Al,) is also constant. | For an $\Omega_m=1$ universe, $\delta_c \approx 1.68$ is constant in time, so $\sigma(M_*)$ is also constant. |
This means M,°xe. Wor. | This means $M_*^{n+3 \over 6} \propto a$. |
ds fixed in time. CXFueX0 follows from the definitions of e and rj and [rom pra"7. | If $r_s$ is fixed in time, $c \propto r_{\rm vir} \propto a$ follows from the definitions of $c$ and $r_{\rm vir}$ and from $\bar\rho \propto a^{-3}$. |
Since exAL,© then 3nod M we assume A is constant. | Since $c \propto M_*^{-\beta}$ then $
\beta \approx -{n+3 \over 6}$ if we assume $M$ is constant. |
In reality AZ also increases Swith a. which decreases 3 somewhat. although not bv more than 20%. | In reality $M$ also increases with $a$, which decreases $\beta$ somewhat, although not by more than . |
. We caleulated halo model power spectra with m=.—2.0 and = L5.for which 3=—0.16 and —0.25 as caleulated above. with several values of ey. | We calculated halo model power spectra with $n=-2.0$ and $n=-1.5$, for which $\beta=-0.16$ and $-0.25$ as calculated above, with several values of $c_0$. |
Ehese spectra are shown in Figure 2.. | These spectra are shown in Figure \ref{fig:scalefree}. |
The agreement is quite good. given. all the limitations of the halo model. | The agreement is quite good, given all the limitations of the halo model. |
At higher & in the n=2.0 case. it appears that the slope of the power spectrum disagrees independent of eo. | At higher $k$ in the $n=-2.0$ case, it appears that the slope of the power spectrum disagrees independent of $c_0$ . |
For Affe2 this model is better fit by a power spectrum with 3=037. ο= 2.6. | For $k/k_*>2$ this model is better fit by a power spectrum with $\beta=-.037$, $c_0=2.6$ . |
However. according to figure 12 of ?.. simulation cata do not exist for Αν greater than a few tens in the n=2 case. so the discrepancy is not really significant. | However, according to figure 12 of \citet{2002astro.ph..7664S},, simulation data do not exist for $k/k_*$ greater than a few tens in the $n=-2$ case, so the discrepancy is not really significant. |
Inthe n=1.5 case. which is tested against simulations to Ah.= 100. the | Inthe $n=-1.5$ case, which is tested against simulations to $k/k_*=100$ , the |
Strip. | Strip. |
These were (observation numbers 0127921001(GWS1), 0127921101(GWS2) and 0127921201(GWS3)) and the first two were reported to have enhanced OVII and OVIII emission (correlated with enhanced solar wind flux as compared to a low solar proton flux for GWS3). | These were (observation numbers 0127921001(GWS1), 0127921101(GWS2) and 0127921201(GWS3)) and the first two were reported to have enhanced OVII and OVIII emission (correlated with enhanced solar wind flux as compared to a low solar proton flux for GWS3). |
GWSI (case {12}) and GWS2 (case (9]) had | GWS1 (case $\{12\}$ ) and GWS2 (case $\{9\}$ ) had |
of studying this state experimentally? | of studying this state experimentally? |
The big bane theory [or the creation and evolution of our universe implies (hat in its early stages. it must have consisted of deconfined quark and egluons. | The big bang theory for the creation and evolution of our universe implies that in its early stages, it must have consisted of deconfined quark and gluons. |
Neutron stars consist of very dense nuclear matter. and it is conceivable that they have quark matter cores. | Neutron stars consist of very dense nuclear matter, and it is conceivable that they have quark matter cores. |
Both these possible applications are interesting. vet they do nol really allow a svstematic study. | Both these possible applications are interesting, yet they do not really allow a systematic study. |
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