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The pulse broadening is measured bv fitting the convolution of a Gaussian template pulse with a truncated exponent as the thin screen scatter function. to the observed pulsar pulse. | The pulse broadening is measured by fitting the convolution of a Gaussian template pulse with a truncated exponent as the thin screen scatter function, to the observed pulsar pulse. |
The results of these measurements over a period of G00 davs are shown in Figure 2.. | The results of these measurements over a period of 600 days are shown in Figure \ref{fig:dmscat}. |
This shows a cliscrete event. lasting 200 davs (ALJD 53950 51150). during which the dispersion aud scattering changed together. | This shows a discrete event, lasting 200 days (MJD 53950 – 54150), during which the dispersion and scattering changed together. |
The two curves are shown as recorded: note especially the sharp rise at the start of the event. aud the delay of 30 davs between the ouset of the rise in scattering aud the rise 1u DM. | The two curves are shown as recorded; note especially the sharp rise at the start of the event, and the delay of 30 days between the onset of the rise in scattering and the rise in DM. |
Both before aud afer this event there are smaller variations which are less obviously correlated. | Both before and after this event there are smaller variations which are less obviously correlated. |
The event appears as a distinct phenomenon which stands out from the ecnueral level of variation iu both parameters. | The event appears as a distinct phenomenon which stands out from the general level of variation in both parameters. |
The dispersion nieasure is proportional to the total electron coutent along the line of sight. | The dispersion measure is proportional to the total electron content along the line of sight. |
Most of this is attributed to the interstellar medimu. aud this componcut is not expected to show such large aud rapid variations: observations of other pulsars show only comparatively sunall and slow variations. as shown bv ?.. | Most of this is attributed to the interstellar medium, and this component is not expected to show such large and rapid variations: observations of other pulsars show only comparatively small and slow variations, as shown by \cite{you07}. |
The base level of the dispersion mcasure appears to be 56715 pe: the event increases this by ADAI z 0.03 bpe. | The base level of the dispersion measure appears to be 56.745 $^{-3}$ pc; the event increases this by $\Delta$ DM $\approx$ 0.03 $^{-3}$ pc. |
The observed scattering. by contrast. is more than doubled at the event. increasiug from 10 to 25 is. | The observed scattering, by contrast, is more than doubled at the event, increasing from 10 to 25 ms. |
Scattering bv radon variations in refractive iudex depends on irregular fluctuations of electron deusitv within anv part of the propagation path: the simplest interpretation is that the increased scattering aud the increased dispersion are both due to a discrete electron. cloud or filament within the Nebula. | Scattering by random variations in refractive index depends on irregular fluctuations of electron density within any part of the propagation path; the simplest interpretation is that the increased scattering and the increased dispersion are both due to a discrete electron cloud or filament within the Nebula. |
Three leneth scales are involved in estimating the size of a sinele cloud respousible both for mereased dispersion andscatterme: | Three length scales are involved in estimating the size of a single cloud responsible both for increased dispersion andscattering: |
they are indeed observed allows us to conclude that Rina,> A. | they are indeed observed allows us to conclude that $R_{\rm{max}} > A$ . |
Nevertheless. we cannot discard a possible relationship between truncations and warps. | Nevertheless, we cannot discard a possible relationship between truncations and warps. |
It appears that optical warps always start closer in than HI warps. although we note that the low resolution of the HI data makes it difficult to detect warps. | It appears that optical warps always start closer in than HI warps, although we note that the low resolution of the HI data makes it difficult to detect low-amplitude warps. |
Low luminosity gamma-ray bursts (LGIhRDs) constitute a sub-class of eanmnma-rav bursts (GRBs) that plavs a central role in the GRD-supernova connection. | Low luminosity gamma-ray bursts () constitute a sub-class of gamma-ray bursts (GRBs) that plays a central role in the GRB-supernova connection. |
While/-GRBs differ from typical long GRBs (LGRBs) in many aspects. (μον also share some common features. | While differ from typical long GRBs (LGRBs) in many aspects, they also share some common features. |
Therefore. the question whether ihe gamma-ray emission of/-GRBs and LGRBs has a common origin is of great interest. | Therefore, the question whether the gamma-ray emission of and LGRBs has a common origin is of great interest. |
Llere we address this question by testing whether/-GRBs. like LGRBs according to the Collapsar model. can be generated by relativistic jets that punch holes in the envelopes of (heir progenitor stars. | Here we address this question by testing whether, like LGRBs according to the Collapsar model, can be generated by relativistic jets that punch holes in the envelopes of their progenitor stars. |
The collapsar model predicts (hat the durations of most observed bursts will be comparable to. or longer than. the lime it takes the jets to breakout of the star. | The collapsar model predicts that the durations of most observed bursts will be comparable to, or longer than, the time it takes the jets to breakout of the star. |
We calculate the jet breakout (times of/EGRBs and compare them to the observed duratons. | We calculate the jet breakout times of and compare them to the observed durations. |
We find that there is a significant. access of/-GRBs with durations that are much shorter than the jet breakout time and (hat these are inconsistent with the Collapsar model. | We find that there is a significant access of with durations that are much shorter than the jet breakout time and that these are inconsistent with the Collapsar model. |
We conclude that the processes (hat dominate (he eamama-ray eniission of/-GIDs and of LGRBs are most likely fundamentally different. | We conclude that the processes that dominate the gamma-ray emission of and of LGRBs are most likely fundamentally different. \end{abstract}\tikzmark{mainBodyEnd184}
\tikzmark{mainBodyStart185}\begin{document} |
According to the Collapsar model (Paczenski19938:MacFadyen&Woosley1999) (he core collapse of a massive star results in the Formation of a compact object. a black hole or a rapidly rotating neutron star. | According to the Collapsar model \citep{Paczynski98,MacFadyen99} the core collapse of a massive star results in the formation of a compact object, a black hole or a rapidly rotating neutron star. |
The compact object ejects a relativistic bipolar. barvon poor jel. along ils rotation axis. | The compact object ejects a relativistic bipolar, baryon poor jet, along its rotation axis. |
The jet punctures the surrounding stellar envelope and it emits the observed 5-ravs at a laree distance from (he star where the optical depth is small aud the high energy photons can escape. | The jet punctures the surrounding stellar envelope and it emits the observed $\gamma$ -rays at a large distance from the star where the optical depth is small and the high energy photons can escape. |
This model. (hat is accepted as the standard model for long GRBs (LGRBs). explains naturally the association of some LGRDs with SNe. aud (heir general emergence in star forming regions reviews).. | This model, that is accepted as the standard model for long GRBs (LGRBs), explains naturally the association of some LGRBs with SNe, and their general emergence in star forming regions \citep[see][for recent reviews]{Woosley06, Hjorth11}. . |
(MeClintock&Remillard2004... <10 1) Williamsetal.2004:DiStefano2002:Trudolvuboyetal.2001:Osborne (Williamsetal.2005a.b.c..2004).. | \citealp{mcclintock2004}, $\gap10^{38}$ $^{-1}$ \citealp{williams2004hrc,distefano2004,kong2002acis,trudolyubov2001,osborne2001}; \citep{williams2005bh1,williams2005bh2,williams2005bh4,williams2004hrc}. |
(Mereghetti 2008:: Camiloetal.2007a:; Halpernetal.2005)) in quiescence and larger ratios in outburst. | \citealp{Mer08}; ; \citealp{CamApJ666}; \citealp{Hal05}) ) in quiescence and larger ratios in outburst. |
The radio emission from 1510-197 was discovered immediately following a strong X-ray outburst. | The radio emission from J1810–197 was discovered immediately following a strong X-ray outburst. |
It has since faded. both in the radio and the X-ray band. and the radio pulsations are no longer visible. | It has since faded, both in the radio and the X-ray band, and the radio pulsations are no longer visible. |
For 11547-5408. the radio emission is also highly variable and appears to be revived in the periods after its X-ray outbursts. | For 1547–5408, the radio emission is also highly variable and appears to be `revived' in the periods after its X-ray outbursts. |
PSR 11622-4950 on the other hand. has had at least two episodes of non-detections in the radio band lasting hundreds of days followed by periods of bright radio emission (see Fig. 1)). | PSR J1622–4950 on the other hand, has had at least two episodes of non-detections in the radio band lasting hundreds of days followed by periods of bright radio emission (see Fig. \ref{Fig:Lightcurve}) ). |
In addition to the new observation. we searched archival data fromChandra...Newton...Rosat.. ASCA.. Beppo-SAX..Rossi-XTE and for an outburst. however no evidence for X-ray flux variability and no X-ray outburst at the level of the outbursts seen in [1810-197 and 11547—5408 in connection to the radio pulsations C7. 1079 ss!) were found since at least as early as 2005. | In addition to the new observation, we searched archival data from, and for an outburst, however no evidence for X-ray flux variability and no X-ray outburst at the level of the outbursts seen in 1810–197 and 1547–5408 in connection to the radio pulsations $\gtrsim$ $^{36}$ $^{-1}$ ) were found since at least as early as 2005. |
It is possible therefore that an enhancement of X-ray activity is not a requirement for pulsed radio emission by magnetars. however. given the duty cycle of sensitive X-ray observations of the field containing JJ1622—4950. we cannot constrain the occurrence of fainter X-ray enhancements of the source. | It is possible therefore that an enhancement of X-ray activity is not a requirement for pulsed radio emission by magnetars, however, given the duty cycle of sensitive X-ray observations of the field containing J1622–4950, we cannot constrain the occurrence of fainter X-ray enhancements of the source. |
What is instead certain is that the observed X-ray emission from JJ1622—4950 is at variance with what is observed for the other two radio pulsating magnetars. | What is instead certain is that the observed X-ray emission from J1622--4950 is at variance with what is observed for the other two radio pulsating magnetars. |
If the true age of PSRJJI622—4950 Is similar to its characteristic age of 4kkyr. we might expect to see a supernova remnant (SNR) surrounding the pulsar. | If the true age of J1622–4950 is similar to its characteristic age of kyr, we might expect to see a supernova remnant (SNR) surrounding the pulsar. |
Indeed. 5 of the 9 AXPs and at least 1 of the 5 SGRs are located within SNRs (Mereghetti2008:: Gaensleretal. 2001)). | Indeed, 5 of the 9 AXPs and at least 1 of the 5 SGRs are located within SNRs \citealp{Mer08}; \citealp{Gae01}) ). |
Inspecting the ATCA image in Fig. 2.. | Inspecting the ATCA image in Fig. \ref{Fig:ATCA-CXO}, |
we seea ring of emission centered ~2' south of the pulsar location. | we seea ring of emission centered $\sim$ $'$ south of the pulsar location. |
This ring lacks an infra-red counterpart and appears to be non thermal. whereas the extended radio source to the south of the ring is clearly thermal in nature. | This ring lacks an infra-red counterpart and appears to be non thermal, whereas the extended radio source to the south of the ring is clearly thermal in nature. |
Could the ring be the SNR and the pulsar has escaped its bounds? | Could the ring be the SNR and the pulsar has escaped its bounds? |
If we assume a distance of ~9 kkpe to the magnetar and further assume 1t was born in the centre of the ring. the magnetar would need a velocity of ~1300kkm ss! to reach its current location whereas the ring itself would have a lower expansion velocity. | If we assume a distance of $\sim$ kpc to the magnetar and further assume it was born in the centre of the ring, the magnetar would need a velocity of $\sim$ $^{-1}$ to reach its current location whereas the ring itself would have a lower expansion velocity. |
Such a velocity is high (though not impossible) for pulsars but rather low for expanding SNRs. | Such a velocity is high (though not impossible) for pulsars but rather low for expanding SNRs. |
Although the link between the ring and the magnetar Is a possibility we consider it unlikely. | Although the link between the ring and the magnetar is a possibility we consider it unlikely. |
The HTRU survey has discovered a radio-luminous pulsar. which is highly polarized. has an inverted spectrum. and is highly variable 1n. both its pulse profile and flux density. | The HTRU survey has discovered a radio-luminous pulsar, which is highly polarized, has an inverted spectrum, and is highly variable in both its pulse profile and flux density. |
The radio pulsar has a faint X-ray counterpart that appears to be stable in flux. with a value that is typical of a quiescent magnetar. | The radio pulsar has a faint X-ray counterpart that appears to be stable in flux, with a value that is typical of a quiescent magnetar. |
The pulsar shares many of the properties of the two known radio magnetars and we therefore conclude that JJ1622—4950 is indeed a magnetar. the first discovered through its radio emission. | The pulsar shares many of the properties of the two known radio magnetars and we therefore conclude that J1622–4950 is indeed a magnetar, the first discovered through its radio emission. |
This discovery not only adds a new member to the magnetar family. but also highlights unprecedented features of the emission of the magnetars across the electromagnetic band. | This discovery not only adds a new member to the magnetar family, but also highlights unprecedented features of the emission of the magnetars across the electromagnetic band. |
At odds with what is observed in other sources. JJ1622-4950 indicates that bright radio emission can be present even when a magnetar displays an X-ray luminosity typical of a quiescent state. | At odds with what is observed in other sources, J1622–4950 indicates that bright radio emission can be present even when a magnetar displays an X-ray luminosity typical of a quiescent state. |
Moreover. JJ1622-4950 shows that radio emission can either exist without the occurrence of a strong X-ray outburst. or occur a long time (2 5 years) after the outburst. | Moreover, J1622–4950 shows that radio emission can either exist without the occurrence of a strong X-ray outburst, or occur a long time $\gtrsim$ 5 years) after the outburst. |
Alternatively. the radio pulsations could be triggered by a modest increment of X-ray activity. that escaped detection in this case. | Alternatively, the radio pulsations could be triggered by a modest increment of X-ray activity, that escaped detection in this case. |
We finally note that the extreme variability in the flux density of JJ1622—4950 also demonstrates the advantages of surveying the radio sky at regular intervals with even modest sensitivity. | We finally note that the extreme variability in the flux density of J1622–4950 also demonstrates the advantages of surveying the radio sky at regular intervals with even modest sensitivity. |
This highlights the potential of the upcoming radio facilities like the LOFAR. ASKAP or the SKA which promise to characterize the dynamie radio sky at an unprecedented level. | This highlights the potential of the upcoming radio facilities like the LOFAR, ASKAP or the SKA which promise to characterize the dynamic radio sky at an unprecedented level. |
The Parkes Observatory and the Australia Telescope Compact Array are part of the Australia Telescope. which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. | The Parkes Observatory and the Australia Telescope Compact Array are part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. |
The ChandraX-ray Observatory Centre is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NASS03060. | The ChandraX-ray Observatory Centre is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. |
This work is partly supported by the Australian Research Council through its discovery programme. | This work is partly supported by the Australian Research Council through its discovery programme. |
The HYDRA supercomputer at the JBCA is supported by a grant from the UK Science and Technology Facilities Council. | The HYDRA supercomputer at the JBCA is supported by a grant from the UK Science and Technology Facilities Council. |
S.B. gratefully acknowledges the support of STFC in his PhD studentship. | S.B. gratefully acknowledges the support of STFC in his PhD studentship. |
This work is partly supported by theAustralian Research Couneil through its discovery programme. Parkes.. ATCA.. (ASIS-D.. | This work is partly supported by theAustralian Research Council through its discovery programme. , , . |
“classical” LBCs like QU317-383 C5. but also galaxies selected with other UV-based criteria. | “classical” LBGs like Q0347-383 C5, but also galaxies selected with other UV-based criteria. |
Overall. this illustrates the difficulties related to purely morphological aud photometric studies and lighlielts the need to iuclude inteeral-field kinciatics for statistically robust samples of the various lLiel-vedshift ealaxy populations. if we want to understaud the wuderlving mechanisius governing galaxy evolution iu the carly wniverse. | Overall, this illustrates the difficulties related to purely morphological and photometric studies and highlights the need to include integral-field kinematics for statistically robust samples of the various high-redshift galaxy populations, if we want to understand the underlying mechanisms governing galaxy evolution in the early universe. |
We presented an analysis of rest-frame optical iuteeral-field spectroscopy of the +=3.23 Lyiman-Break Calaxy QO317-383 C5 in he I baud. | We presented an analysis of rest-frame optical integral-field spectroscopy of the $z=3.23$ Lyman-Break Galaxy Q0347-383 C5 in the K band. |
This galaxy is oue of the largest 1-1i0wn LBGs. and iu particular large enough for secine-limited observations. | This galaxy is one of the largest known LBGs, and in particular large enough for seeing-limited observations. |
QU317-383 C5 was first described by ?.. who obtained E702W IIST continua oeuaeiue aud longsli spectroscopy in the I-baud We detect the |OTMJAA 959.5007 doublet with line oxoperties that are similar to those discussed in ?.. but oe1 addition. we also identify with a flux of 9«10.008 erg I 7. | Q0347-383 C5 was first described by \citet{pettini01}, who obtained F702W HST continuum imaging and longslit spectroscopy in the K-band We detect the $\lambda\lambda$ 4959,5007 doublet with line properties that are similar to those discussed in \citet{pettini01}, but in addition, we also identify $\beta$ with a flux of $9\times10^{-18}$ erg $^{-1}$ $^{-2}$. |
The [OTII[/TI./ line ratio is high. o»ut not oo high for a low-nctalicity star-forming ogalaxy. aud corresponds to an oxvgen abundance within the range of uetallicities of LBGs measured by ?.. | The $\beta$ line ratio is high, but not too high for a low-metalicity star-forming galaxy, and corresponds to an oxygen abundance within the range of metallicities of LBGs measured by \citet{pettini01}. |
The observations do tot sugeest that the optical spectrum of QUJ17-383 C5 is dominated by an ACN. | The observations do not suggest that the optical spectrum of Q0347-383 C5 is dominated by an AGN. |
The |OIH]A5007 line image shows two knots at a xojected distance ~0.7 ((5.L kpe) with a small relative velocity of 33 kan |. | The $\lambda$ 5007 line image shows two knots at a projected distance $\sim 0.7$ (5.4 kpc) with a small relative velocity of 33 km $^{-1}$. |
Line morphology aud sincluatics do not resemble those expected for au outflow or a rotating disk. and more ikely originate from a merger of either two imtermeciate-nass galaxies with a dvuamical mass of ΠΑΕ, each. or perhaps massive sub-chuups of a fragmented disk as ostulated by οον, | Line morphology and kinematics do not resemble those expected for an outflow or a rotating disk, and more likely originate from a merger of either two intermediate-mass galaxies with a dynamical mass of $\le 10^{10} M_{\odot}$ each, or perhaps massive sub-clumps of a fragmented disk as postulated by \citet{immeli04,bournaud07}. |
The arge inasses of individual knots uake it more likely that we see the merging of two galaxies cach tracing its individual dark matter halo or subhalo. although this is a very difficult distinction to make with oxeseut dav data. | The large masses of individual knots make it more likely that we see the merging of two galaxies each tracing its individual dark matter halo or subhalo, although this is a very difficult distinction to make with present day data. |
The density of simularly huninous z~3 LBCes is consistent with predictions frou recent models of the cosmic evolution of the moereer rate. | The density of similarly luminous $\sim 3$ LBGs is consistent with predictions from recent models of the cosmic evolution of the merger rate. |
Stary-formation rates estimate from the observed IL? flux correspond to ~20LO AL. in each clamp. which is uot unusual for LDCs ecnerally. | Star-formation rates estimated from the observed $\beta$ flux correspond to $\sim 20-40$ $_{\odot}$ in each clump, which is not unusual for LBGs generally. |
Most z—23 LBCs are significantly more compact than QO3L7-38e C5. with typical halflight radi of rs~0.37. | Most $\sim 3$ LBGs are significantly more compact than Q0347-388 C5, with typical half-light radii of $_e\sim 0.3$. |
Such scales are difficult to resolve with 1ni class telescopes. even with adaptive optics assisted observations. | Such scales are difficult to resolve with 10-m class telescopes, even with adaptive optics assisted observations. |
From. such observations 7? find that DSF2237a-C?2. their only target at z»3. has a velocity eracdicent aud velocity dispersions of the same magnitude as the shear. | From such observations \citet{law07} find that DSF2237a-C2, their only target at $>$ 3, has a velocity gradient and velocity dispersions of the same magnitude as the shear. |
While superficially these characteristics could be suggestive of a rotating disk. ?.. from a comparison of their data to a simple exponeutial rotating disk model. cluphasize that this source is unlikely to be a thin. rotationallv-supported disk. | While superficially these characteristics could be suggestive of a rotating disk, \citet{law07}, from a comparison of their data to a simple exponential rotating disk model, emphasize that this source is unlikely to be a thin, rotationally-supported disk. |
Both ealaxics are among the lareest LBCs aud are comparably bright. which sheds doubts as to whether the properties of the overall population of :~3 LDGs are well described by the properties of its largest members. | Both galaxies are among the largest LBGs and are comparably bright, which sheds doubts as to whether the properties of the overall population of $z\sim 3$ LBGs are well described by the properties of its largest members. |
?— found evidence for rotatiou on sub-kpe scales iu a stronely-lensed LDC: at z=3.2L. but such scales are well bevond reach for eecnerie LDGs even with adaptive optics. | \citet{nesvadba06} found evidence for rotation on sub-kpc scales in a strongly-lensed LBG at $=3.24$, but such scales are well beyond reach for generic LBGs even with adaptive optics. |
While adaptive optics-assisted observations allow to probe the dyvuamics of lhiel-redshift galaxies at sub-kpe resolution. they niust concentrate ou galaxies with particularly bright line enission. to eusure reasonable observing times as poiuted out bv ?.. | While adaptive optics-assisted observations allow to probe the dynamics of high-redshift galaxies at sub-kpc resolution, they must concentrate on galaxies with particularly bright line emission, to ensure reasonable observing times as pointed out by \citet{law07}. |
This will inevitably lead to biases between observed LBC samples aud the pareut population of LBGs. aud Is a reason why studies of eravitationally leused are not superceded. but are rather complemented. bv high aneular resolution observations of LBCs with adaptive optics. in spite of uucertaiuties related to the eravitationa magnification. | This will inevitably lead to biases between observed LBG samples and the parent population of LBGs, and is a reason why studies of gravitationally lensed are not superceded, but are rather complemented, by high angular resolution observations of LBGs with adaptive optics, in spite of uncertainties related to the gravitational magnification. |
More positively. observing galaxies with bright line cussion will plausibly provide information about particularly rapid phases of star-formation ac ealaxv growth. whatever mechanisni is responsible for initiating such phases; | More positively, observing galaxies with bright line emission will plausibly provide information about particularly rapid phases of star-formation and galaxy growth, whatever mechanism is responsible for initiating such phases. |
Prudenuce aud caution however are certainly justified when ecueralizing the results of lugh redshift geealaxics eiven the current liuitatiou iu astronomical instrmucutation aud the small sample sizes with detailed 3-dimensioual spectroscopy observations. | Prudence and caution however are certainly justified when generalizing the results of high redshift galaxies given the current limitation in astronomical instrumentation and the small sample sizes with detailed 3-dimensional spectroscopy observations. |
We would like to thank an anonymous referee for. helpfi advice and suggestions that substantially. improved this paper and the stall at Paranal for their help and. suppor in obtaining these observations. | We would like to thank an anonymous referee for helpful advice and suggestions that substantially improved this paper and the staff at Paranal for their help and support in obtaining these observations. |
ΝΡΗΝ wishes to acknowledge financial support from. the European Commission through a Marie. Curie Postdoctoral Fellowship and MDL wishes to thank the Centre Nationale de Ia Recherche Scientifique for its continuing support of his research. | NPHN wishes to acknowledge financial support from the European Commission through a Marie Curie Postdoctoral Fellowship and MDL wishes to thank the Centre Nationale de la Recherche Scientifique for its continuing support of his research. |
and helium ionization degrees of jjj=0.8 and Oy.=O.1. respectively. | and helium ionization degrees of $\mutilde_{\rm H} = 0.8$ and $\delta_{\rm He}=0.1$, respectively. |
We see that even in the case of the largest quantity of helium considered (£j,=20%). the presence of helium has a minor effect on the results. | We see that even in the case of the largest quantity of helium considered $\xi_\ion{He}{i} = 20\%$ ), the presence of helium has a minor effect on the results. |
In the case of Alfvénn and fast waves (Fig. | In the case of Alfvénn and fast waves (Fig. |
2aa.b). their critical wavenumber (1.e.. the value of & which causes the real part of the frequency to vanish) is shifted toward slightly smaller values. | \ref{fig:mhdwaves}a a,b), their critical wavenumber (i.e., the value of $k$ which causes the real part of the frequency to vanish) is shifted toward slightly smaller values. |
So. the larger ἕμοι. the smaller K?. | So, the larger $\xi_\ion{He}{i}$, the smaller $k_{\rm c}^{\rm a}$. |
This result can be understood by considering that the Alfvénn wave critical wavenumber. κά, given by Eq. ( | This result can be understood by considering that the Alfvénn wave critical wavenumber, $k_{\rm c}^{\rm a}$ , given by Eq. ( |
38) of Is. with v4=Bo/Vipo the Alfvénn speed. | 38) of \citet{forteza08} is, with $\va = B_0 / \sqrt{\mu \rho_0}$ the Alfvénn speed. |
Equation (21)) is also approximately valid for the fast wave critical wavenumber. | Equation \ref{eq:crit}) ) is also approximately valid for the fast wave critical wavenumber. |
Then. we see that K? is inversely proportional to Cowling's diffusivity. ic. | Then, we see that $k_{\rm c}^{\rm a}$ is inversely proportional to Cowling's diffusivity, $\eta_{\rm C}$. |
Since jc is larger in the presence of helium than in the pure hydrogen case due to additional collisions of neutral andsingly ionized helium species. ko is therefore smaller. | Since $\eta_{\rm C}$ is larger in the presence of helium than in the pure hydrogen case due to additional collisions of neutral andsingly ionized helium species, $k_{\rm c}^{\rm a}$ is therefore smaller. |
Turning our attention to the slow wave (Fig. | Turning our attention to the slow wave (Fig. |
2cc). we see that the maximum and the right-hand side minimum of rp/P are also slightly shifted toward smaller values of κ. | \ref{fig:mhdwaves}c c), we see that the maximum and the right-hand side minimum of $\tdp$ are also slightly shifted toward smaller values of $k$. |
Results from Carbonellet and Fortezaetal.(2008) indicate that thermal conduction is responsible for these maximum and minimum of rp/P. | Results from \citet{carbonell04} and \citet{forteza08} indicate that thermal conduction is responsible for these maximum and minimum of $\tdp$. |
Thus. the additional contribution of neutral helium atoms to thermal conduction (Eq. 19)) | Thus, the additional contribution of neutral helium atoms to thermal conduction (Eq. \ref{eq:cond}) ) |
causes this displacement of the curve of r5/P. | causes this displacement of the curve of $\tdp$. |
As for Alfvénn and fast waves. this effect is of minor importance. | As for Alfvénn and fast waves, this effect is of minor importance. |
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