Veritas Free Download Key Serial Number LINK

<div>The wait time has become ridiculous. The last contact with me was supp=
osed to be Nov 2nd.</div><div></div><div>Today, I tried calling the 1-866-8=
37-4827 and direct number 1-866-837-4827.</div><div></div><div>I was discon=
nected whether I used 1 for tech support or didn't use 1 and waited on the =
line.</div><div></div><div>If I choose 1 for for tech support, then 1 for U=
S Federal Agency - then I get a prompt for a case number before being disco=
nnected.</div><div></div><div></div><div></div><div></div><div></div><div>V=
eritas Free Download Key Serial Number</div><div></div><div>Download File: =
https://t.co/6Tty1Hpx3R </div><div></div><div></div><div>Good Grief - I jus=
t figured out that Veritas is screening on the phone number that you call f=
rom.</div><div></div><div>I was using a land line that is not my office lan=
d line and tried using my mobile number - and got thru.</div><div></div><di=
v></div><div>Running Veritas BUE v16 and encountering an issue when backing=
 up servers that have a large number of small files. For example, one of ou=
r file servers has 4.3 million files (mostly Office docs, jpg, etc.) in 600=
K folders for a total size of 1.1TB. This takes 18 hours to backup to disk =
at a rate of 1127MB/min. We do this job once a week, then run nightly diffe=
rential backups against it through the rest of the week. For this disk-to-d=
isk job, we aren't doing compression or encryption. This is not an abnormal=
 issue with this one job. We have another job of similar size and file comp=
osition that takes 14 hours to complete. Jobs of similar overall size, that=
 are setup to backup entire VM's take 1/2 the time to complete.</div><div><=
/div><div></div><div>That's what I was fearing the issue was, but hoping th=
at maybe there was a setting I'm missing in the job configuration. On these=
 two servers with the large number of files, we do a full VM backup on Satu=
rday, but then we have to do a data-only backup on Monday so we can have th=
at base-line backup for the differentials. Guess my best bet is to tweak th=
e schedule a bit and do the full data-only backup early Sunday morning so i=
t doesn't overlap into the work week.</div><div></div><div></div><div>I'm r=
unning Veritas Backup Exec v20 and I'm having issues when backing up File s=
erver that have a large number of small files (excel , word ,pp ,pdf ,pictu=
res and video files). Its taking 3 days to backup the 3 TB server at a rate=
 of 616.00MB/min -I have tried to defragment/check disk and reconfigure the=
 job, increase memory on the File and backup server ,check disk on the Hype=
r-V but no joy .When I do a copy 3GB file from the backup server to the fil=
e server it take 4mins or less. Both the File and Backup server are sitting=
 on the same Hyper-V with fibre NIC ,I notice that it's only slow when back=
ing up the small files only on D:</div><div></div><div></div><div></div><di=
v></div><div></div><div></div><div>I haven't seen a way to get the part num=
ber of an appliance drive. The closest I can get is getting the drive seria=
l number and firmware version. This is via the Appliance Web Interface. Go =
to Monitor->Hardware, and then click on Disk (either the one for the head u=
nit, or external storage trays). This will list the drives, including seria=
l number and firmware version.</div><div></div><div></div><div>Call Home is=
n't required for NetBackup Appliances but is highly recommended by Veritas.=
 Regarding Appliance part numbers, from what I know Veritas don't publish t=
hese but customers can purchase spare disks if they want via Veritas sales =
or a partner. However the normal procedure for Appliance hardware failures =
is for Veritas Technical Support to verify Appliance details and the actual=
 failure and then organise the correct replacement and fitting. For very se=
cure environments I heard Technical Support can talk through a customer per=
forming certain part replacements themselves. BR Andrew</div><div></div><di=
v></div><div>I've been asked by our data center manager to provide the tota=
l number of tapes that might be needed for backup for next month. We do get=
 automatic e-mail forecasting for the tape requirement but I've been advise=
d that since the automatic e-mail was started we are using approx100 new ta=
pes per week as compared to 40 before. I was wondering if there is a better=
 way to check exactly how much tapes might be needed for backup.</div><div>=
</div><div></div><div></div><div></div><div></div><div></div><div>The compl=
ex dynamics of the Venus atmosphere produces a periodic mass redistribution=
 pattern. Moving atmospheric masses create a time variable modulation of th=
e gravity field of Venus. Said gravity signal depends on the net transport =
of mass across the globe and on the response of the solid body to the atmos=
phere loading its crust. The gravitational response to the atmospheric load=
ing, parametrized through the loading Love numbers kl', depends on the inte=
rior structure of the planet, most notably on the viscosity of the mantle. =
Measuring the loading Love numbers of Venus would provide new and supplemen=
tary constraints for its interior structure determination.</div><div></div>=
<div></div><div></div><div>he upcoming NASA VERITAS mission to Venus, will =
be capable of determining the gravity field of the planet to unprecedented =
level of detail, and will be sensitive to the gravitational contribution of=
 the atmosphere. We have tested the prospect of measuring Venus' loading Lo=
ve numbers with VERITAS for understanding first if such a measurement is po=
ssible, and secondly what would it imply for the efforts of constraining Ve=
nus' deep interior structure.</div><div></div><div></div><div></div><div></=
div><div></div><div>Figure 1. Amplitude spectra of the Venus gravity field =
measured by Magellan and the associated uncertainty (black solid and dashed=
 lines, respectively), the predicted uncertainty on the gravity field measu=
red by VERITAS (blue dash-dotted line) and the amplitude of the gravity fie=
ld induced by atmospheric mass redistribution (red line). The lowest degree=
s of the atmospheric field are above the VERITAS noise floor.</div><div></d=
iv><div></div><div></div><div></div><div></div><div>Figure 2. Atmospheric p=
ressure anomalies over one Venus solar day. The pressure field has been obt=
ained from [Garate-lopez et al., 2018].</div><div></div><div></div><div></d=
iv><div>The first task to be addressed, for answering these questions, cons=
ists in understanding the dependence of the Love numbers to the interior st=
ructure of Venus. To this aim we have calculated the tidal and loading Love=
 numbers of Venus based on the latest interior models proposed in literatur=
e (notably by Dumoulin et al., 2017 and Xiao et al., 2021). These models va=
ry interior density distributions, viscosity profiles, core radius and core=
 status (solid/liquid) allowing us to assess the relation between these qua=
ntities and the load Love numbers. The Love numbers have been computed usin=
g the TidalPy library which solves the viscoelastic-gravitational problem u=
sing the shooting method. The shooting method readily allows for the effect=
s due to compressibility to be explored in a computationally stable way. We=
 have found compressibility to be an important factor for a planet like Ven=
us, especially for the calculation of the loading Love numbers. By computin=
g the Love numbers on such a wide spectrum of interior models we have asses=
sed the expected ranges of values showing a 34% and 22.5% variation in the =
tidal Love number k2 and 43.1% and 22.1% in the loading Love number k2' und=
er the assumption of a liquid and solid core, respectively. We have compute=
d the full set of Love numbers (tidal, loading, and vertical displacement h=
l) up to degree 10 for the hundreds of interior model variations considered=
 (see Data section for more details).</div><div></div><div></div><div></div=
><div></div><div></div><div>Figure 3. Comparison of the computed tidal and =
loading Love numbers under the compressible and incompressible assumptions.=
</div><div></div><div></div><div></div><div></div><div></div><div>Figure 4.=
 Tidal and loading Love numbers values as a function of the degree, with va=
rying assumptions on the mantle viscosity.</div><div></div><div></div><div>=
</div><div>To assess the VERITAS sensitivity to kl' we have run a set of hi=
gh-fidelity numerical simulations reproducing the nominal operational scena=
rio of the gravity science experiment. We have focused on understanding the=
 role that systematic errors, arising from uncertain knowledge of the full =
dynamical environment of the probe, including the planet's static gravity f=
ield and the underlying atmospheric model, could have on the final estimate=
 of the Love numbers (more details can be found in Cascioli et al., 2023).<=
/div><div></div><div></div><div></div><div>We have shown that VERITAS will =
be able to measure k2' to a level of 10%and 4% of the maximum expected rang=
e, when considering Doppler tracking data only and Doppler tracking combine=
d with radar tie points, respectively. Depending on the assumptions, moreov=
er, VERITAS will have sensitivity also to k3' and k4'.</div><div></div><div=
></div><div></div><div>The simultaneous measurement of k2 and k2' define a =
3-dimensional measurement in the phase space of Venus Love numbers, namely =
the real and imaginary portions of the degree-2 tidal Love number at the ti=
dal forcing period of 58.3 days (frequency =CF=89T), and the real portion o=
f the loading Love number. Since the diurnal thermal tides are the principa=
l contribution to the atmospheric loading, the loading Love numbers are ass=
umed to be measured at the solar forcing period of 116.75 days (frequency =
=CF=89_S). In concert, these three values (along with other measurements of=
, e.g., the moment of inertia factor, k3', k4') can be used to determine th=
e most likely interior and thermal state of Venus in both a structural and =
rheological context. In Figure 5, we show how measurements made by VERITAS =
can narrow the most likely mantle viscosity for the planet. The small obser=
vational uncertainties (shown as error bars in the figure) calculated for t=
he real and imaginary tidal Love numbers are small enough for future VERITA=
S measurements to isolate a small number of likely interior models from tho=
se considered by Xiao et al., 2021 and Dumoulin et al., 2017. These two par=
ameters cannot alone capture the entire spectrum of possible models since, =
as shown in Figure 5, this would correspond to projecting the whole model c=
loud onto the (Re[k2], Im[k2]) plane, losing information from the third dim=
ension provided by the loading Love number. The uncertainty in the loading =
Love number, although substantially larger, can further constrain the likel=
y composition, viscosity, as well as other rheological parameters.</div><di=
v></div><div></div><div></div><div></div><div></div><div>Figure 5. Tidal an=
d loading degree-2 Love numbers as a function of mantle viscosity. Error ba=
rs show the VERITAS predicted measurement uncertainty (black: Doppler only,=
 red: Doppler + tie points).</div><div></div><div></div><div></div><div>Thi=
s consideration is particularly true for interior models with low mantle vi=
scosities, where the effects of tidal dissipation become dominant. There ex=
ist well-determined relationships between different sets of Love numbers. F=
or example, Saito (1978) gives:</div><div></div><div>kl' =3D kl - hl (1)</d=
iv><div></div><div>where h is the vertical displacement tidal Love number, =
relating the tidal gravitational perturbation to the radial displacement of=
 the surface of the body (for a given degree l). This relation was obtained=
 under the hypothesis of a purely elastic response of the planet. When cons=
idering the viscoelastic gravitational problem, this relationship is formal=
ly correct only at a given forcing frequency =CF=89:</div><div></div><div>k=
l' (=CF=89) =3D kl (=CF=89) - hl (=CF=89) (2)</div><div></div><div></div><d=
iv></div><div></div><div></div><div>Figure 6 shows the graphical representa=
tion of this equation. It demonstrates that the elastic relation between Lo=
ve numbers does not hold, especially for low values of the mantle viscosity=
. The deviation of the viscoelastic interior model values from the linearit=
y given by the elastic relation, for low viscosity values, makes explicit t=
he importance of an accurate measurement of k2' as the full spectrum of pos=
sible interior models cannot be described with two parameters (linear relat=
ion between real and imaginary Love numbers).</div><div></div><div></div><d=
iv></div><div></div><div></div><div>Figure 6. Graphical representation of E=
quation 2. The diagonal line represents the elastic limit (i.e., Equation 1=
).</div><div></div><div></div><div></div><div></div><div></div><div>Figure =
7. Degree-2 loading Love number amplitudes as a function of the forcing per=
iod, for different rheologic laws. Error bars represent the predicted VERIT=
AS measurement capabilities.</div><div></div><div></div><div></div><div>As =
we discussed, VERITAS will measure the loading Love number at the diurnal f=
orcing frequency =CF=89S. VERITAS will also measure the tidal Love numbers =
k_2 and h_2 at the tidal (semidiurnal) forcing frequency =CF=89T (additiona=
l details in Cascioli et al., 2021).</div><div></div><div>This allows to wr=
ite the relation:</div><div></div><div>k2' (=CF=89T) =3D k2 (=CF=89T) - h2 =
(=CF=89T) (3)</div><div></div><div></div><div></div><div>From which the loa=
ding love number at the tidal frequency k2' (=CF=89_T) can be derived. It i=
s important to underline that the measurement of k2' (=CF=89_T) obtained th=
is way is completely model independent, relying only on the very general as=
sumptions needed to obtain Equation (2). Figure 7 shows how the concurrent =
measurement of k2' at the two frequencies =CF=89T and =CF=89S has the abili=
ty of constraining two points on the amplitude-frequency curve for the load=
ing Love number. We argue that this may help discriminate different rheolog=
ical laws, and ascertain parameters governing a given rheology. The precise=
 quantification of the constraining power of these measurements, in combina=
tion with other key geophysical parameters estimates (such as the MOIF), wo=
uld require a full inversion of the interior structure model of Venus (e.g.=
, using Monte Carlo Markov Chain techniques). This task goes beyond the sco=
pe of this work, and will be part of future focused follow-on investigation=
s.Data</div><div></div><div></div><div></div><div>We release the software a=
nd data produced in this work.</div><div></div><div>The accompanying ZIP ar=
chive (665MB) contains two main folders, one containing the Venus Love numb=
ers (k,h,l,k') for all the interior structure models we tested. The other c=
ontains executable and commented python code able to reproduce and extend t=
he results of this work.</div><div></div><div>Refer to the README files in =
the repository for a detailed description of its content.</div><div></div><=
div></div><div></div><div>The same data files are hosted at Zenodo:</div><d=
iv></div><div>Gael Cascioli et al. (2023), Venus visco-elastic Love numbers=
 [Data set]. In The Planetary Science Journal (1.0, Vol. 4). Zenodo. Usage =
Policy</div><div></div><div>Please cite the following reference when using =
any of these products:</div><div></div><div></div><div></div><div>Cascioli =
et al. (2023), The Planetary Science Journal, doi:10.3847/PSJ/acc73c.</div>=
<div></div><div> dd2b598166</div>