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Subject: STAR Correlations and Fluctuations PWG
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- From: Frank Geurts <geurts AT rice.edu>
- To: "Lisa, Michael" <lisa AT physics.osu.edu>, STAR Correlations and Fluctuations PWG <star-cf-l AT lists.bnl.gov>
- Subject: Re: [Star-cf-l] Extracting Timescales with HBT
- Date: Mon, 23 Aug 2021 12:04:07 -0500
Hi Mike,
Typically dilepton measurements would look at an excess of the short-lived
rho yield w.r.t. the long-lived vector mesons like the omega and phi. The
motivation is that short-lived rho will decay close to its production point
(1.3 fm/c) while the long-lived vector mesons do so much later (>20fm/c).
See e.g. Heinz and Lee in PLB259(1991)162 and more recently Rapp and Van Hees
in PLB753(2016)586.
Especially fig. 3 in Rapp's paper shows how the excess yield tracks with
lifetime. The statistics goals for BES2 aimed at ~15% statistical
uncertainties in this rho-mass range. That more or less sets a minimum of the
sensitivity of a dielectron "lifetime" measurement. We should be able to give
a better indication based on the last 27GeV data which Zaochen is analyzing,
with the caveat that BES2 will allow us to take advantage of the iTPC (i.e.
lowering the electron pT cut-off).
-Frank
> On Aug 23, 2021, at 10:36 AM, Lisa, Michael via Star-cf-l
> <star-cf-l AT lists.bnl.gov> wrote:
>
> Hi Helen,
>
> Thanks for the message. Indeed, I would expect an extended lifetime to
> affect both systems. As for “lifetime,” that word is overused (like
> “error”), so it’s worthwhile to expand a bit.
>
> For the Rout/Rside, we are talking about the emission duration, which has
> been associated with the “cooling time,” a dynamic timescale that may
> correlate with the time for the phase change to occur. To get an absolute
> *lower limit*, one might assume a spherical source with no flow or
> (producing the same effect) opacity. In that case, tau =
> sqrt(Rout^2-Rside^2)/(pT/mT). For the peak shown in our paper, this would
> be something like sqrt(8 fm^2)/0.9 ~ 3 fm/c. That’s pretty low, but keep
> in mind it ignores flow, which we know is pretty big. For anything more
> serious, one needs to turn to the blast wave, which we showed how to do in
> quite some detail in
> https://urldefense.com/v3/__https://arxiv.org/pdf/nucl-th/0312024.pdf__;!!P4SdNyxKAPE!RxsRZlAQAvxIXmN8q9tKjm5pEEeEahGLOY_mPK3FDBGJIpt7la1dN-7gtPms3OUv1Mb3vaM$
> STAR applied this formalism to its *top energy* data in this paper
> https://urldefense.com/v3/__https://arxiv.org/pdf/nucl-ex/0411036.pdf__;!!P4SdNyxKAPE!RxsRZlAQAvxIXmN8q9tKjm5pEEeEahGLOY_mPK3FDBGJIpt7la1dN-7gtPms3OUvCXIQfwQ$
> There, we found an emission duration of 3 fm/c, even when Rout/Rside
> ~unity. This shows the importance of (radial) flow. My preliminary
> estimate (paper in process) is that STARs result at 20 GeV gives about 10
> fm/c. All of these estimates ignore opacity; including opacity would
> increase the lifetime estimate.
>
> Now, “lifetime” is sometimes used to refer to the “evolution time” of the
> system. Here, we see no peaking, just a slow growth of the evolution time
> with collision energy. This is based on Rlong and a formulation that
> assumes boost-invariance (whose validity deteriorates at low energy, of
> course), and strong flow. In figure 10 of STAR’s later paper
> https://urldefense.com/v3/__https://arxiv.org/pdf/1403.4972.pdf__;!!P4SdNyxKAPE!RxsRZlAQAvxIXmN8q9tKjm5pEEeEahGLOY_mPK3FDBGJIpt7la1dN-7gtPms3OUv0Mg21xY$
> you see a value of something like 7 fm/c at BES energies, and 11 fm/c at
> LHC. This should be the time between the onset of boost-invariant flow and
> the peak of emission. It should likewise be considered a lower limit.
>
> You said you had not seen any attempt of this in a long time. I would like
> to point to one more paper that deals extensively with timescales probed by
> HBT. It is in my opinion (as author, ahem) quite good:
> https://urldefense.com/v3/__https://arxiv.org/pdf/1607.06188.pdf__;!!P4SdNyxKAPE!RxsRZlAQAvxIXmN8q9tKjm5pEEeEahGLOY_mPK3FDBGJIpt7la1dN-7gtPms3OUvqhvf73g$
> It shows a completely different analysis that combines anisotropic HBT
> of the transverse radii (Rout and Rside) with the evolution time given by
> the longitudinal radius (Rlong). The very interesting result is that these
> analyses give consistent results for evolution time. I think that is so
> cool! Check out section 5.2 and figure 10.
>
>
> Very good, so much for HBT. Above I gave some quantitative
> estimates/limits for the timescales that might be indicated. Dilepton
> measurements are probably sensitive to the evolution time. What
> quantitative estimates does one extract from this data? That is the only
> way to tell whether the two measurements give a consistent picture. In
> other words, how much increase in lifetime would be required to produce a
> non-flat structure in the dileptons?
>
> Thanks,
> Mike
>
>
>
> --
> Michael Lisa
> Professor of Physics
> The Ohio State University
>
>
> From: Star-cf-l <star-cf-l-bounces AT lists.bnl.gov> on behalf of Helen Caines
> via Star-cf-l <star-cf-l AT lists.bnl.gov>
> Reply-To: Helen Caines <helen.caines AT yale.edu>, STAR Correlations and
> Fluctuations PWG <star-cf-l AT lists.bnl.gov>
> Date: Friday, August 20, 2021 at 10:46 AM
> To: "star-cf-l AT lists.bnl.gov" <star-cf-l AT lists.bnl.gov>
> Subject: [Star-cf-l] Extracting Timescales with HBT
>
> Hi All,
>
> At this week’s LBNL BES workshop there was a brief discussion triggered
> by the difference in shapes of our reported HBT R_out^2 - R_side^2 vs
> sqrt(s) which might be related to an extended emission duration due passing
> through a first order phase transition, and the excess dilepton yield per
> pion which is also theoretically related to the lifetime of the source.
>
> The HBT result shows a wide peak around 20 GeV while the dilepton results
> appear flat. See for example slides 18 and 20 of my presentation here:
> https://drupal.star.bnl.gov/STAR/files/STARPlansBES-II_0.pdf
>
> I know that the two measurements measure different timescales so the
> absolute values don’t need to agree, but I thought both should be sensitive
> to potential extended freeze-outs generated via a first order phase
> transition. I was therefore wondering of this group if we see this HBT
> peaking in other species? Or rather, since the BES-II data are only just
> coming in, will we have the statistic to look at this and is someone
> currently planning to make the measurements?
>
> Also, at the start of RHIC/STAR there were measurements of “total time of
> collision” being extracted from HBT+ spectra blast wave fits. I haven’t
> seen anyone attempting this in quite some time. Is it still considered a
> valid analysis technique? If so and we perform the study do we see a
> similar peaking?
>
> Thanks
>
> Helen
>
> ***********************
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> New Haven, CT 06520
> 203-432-5831
> ***********************
> she/her/hers
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>
>
>
>
>
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-
[Star-cf-l] Extracting Timescales with HBT,
Helen Caines, 08/20/2021
- Re: [Star-cf-l] Extracting Timescales with HBT, Grigory Nigmatkulov, 08/21/2021
- Re: [Star-cf-l] Extracting Timescales with HBT, Roy Lacey, 08/23/2021
-
Re: [Star-cf-l] Extracting Timescales with HBT,
Lisa, Michael, 08/23/2021
- Re: [Star-cf-l] Extracting Timescales with HBT, Roy Lacey, 08/23/2021
- Re: [Star-cf-l] Extracting Timescales with HBT, Frank Geurts, 08/23/2021
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