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7321. http://hea-www.harvard.edu/PINTofALE/pro/obsolete/setcolor.pro
pro setcolor, colors ,icols, rgbfil = rgbfil ,oldr=oldr, oldg = oldg , oldb = oldb ,$ _ref_extra=ex ;+ ;procedure setcolor ; loads specified colors into color table in specified indices ; ;warning ; this routine is being renamed SETKOLOR to avoid conflict with ; JHUAPL routine of the same name. this will disappear very soon, ; and is hanging around only to aid in the transition. ; ;syntax ; setcolor, colors ,icols, rgbfil = rgbfil ,oldr=oldr, ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/obsolete/setcolor.pro -- 5.2 Кб -- 09.02.2001
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7322. http://hea-www.harvard.edu/PINTofALE/pro/lineid_menu.pro
... WVL : Z, ION : Fx : Tmax Trange : [description] : [match]' mtch_item =cw_bgroup(base_mtch,cc,/column,/nonexclusive, uvalue =' mtch_item ',$ /scroll,y_scroll_size=300,x_scroll_size=700,set_ value =oh,$ label_top=label_top) ; menu bar base_mbar=widget_base(base,frame=2,/row,/map, uvalue ='base_mbar') mbar_help=widget_button(base_mbar, value ='HELP', uvalue ='mbar_help') mbar_pars=widget_button(base_mbar, value ='PARAMETERS', ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/lineid_menu.pro -- 17.5 Кб -- 08.02.2001
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7323. http://hea-www.harvard.edu/PINTofALE/doc/RD_LIST.howto
READING IN CUSTOM LINE LISTS (JJD-JanMMI) ====================================================================== ; Playing with line lists, using RD_LINE(), RD_LIST() and CAT_LN(): ; Quick Example ; ; The function RD_LIST() can read in an ascii line list and from this ; can retrieve the appropriate emissivity data from any of the supported ; databases in the same way that RD_LINE() does. ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/doc/RD_LIST.howto -- 3.5 Кб -- 05.02.2001
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7324. http://hea-www.harvard.edu/PINTofALE/doc/TIP_DENSITY_SPEC
; do spectrum synthesis for two different densities, assuming SP_WGRID ; contains wavelength grid bin boundaries. io_ww=sp_wgrid delvar,linespec_linstr ; makes linespec re-read emissivity DB !EDENS=1.e10 @linespec.par linespec_ne10=varsmooth(linespec_spec,5.,type='beta=1.8') delvar,linespec_linstr !EDENS=1.e13 @linespec.par linespec_ne13=varsmooth(linespec_spec,5.,type='beta=1.8')
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Ссылки http://hea-www.harvard.edu/PINTofALE/doc/TIP_DENSITY_SPEC -- 1.4 Кб -- 02.02.2001
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7325. http://hea-www.harvard.edu/PINTofALE/doc/TIP_ABUN_SPEC
; Do line synthesis for solar photospheric, then metal poor [M/H]=-0.5 ; abundances, assuming SP_WGRID contains wavelength grid bin boundaries. ; Default abundances on start-up are Grevesse et al. (1992) - re-read ; just in case io_ww=sp_wgrid !abund=getabund('Grevesse') @linespec.par linespec_0.0=varsmooth(linespec_spec,5.,type='beta=1.8') !abund=getabund('Grevesse',metals=-.5) @linespec.par linespec_ne13=varsmooth(linespec_spec,5.,type='beta=1.8')
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Ссылки http://hea-www.harvard.edu/PINTofALE/doc/TIP_ABUN_SPEC -- 1.4 Кб -- 02.02.2001
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7326. http://hea-www.harvard.edu/PINTofALE/doc/TIP_DB_CHANGE
; Read line emissivities, save the line structure, then change DB and re-read !LDBDIR='$CHIANTI' @rd_line.par linstr_chianti=rd_line_linstr !LDBDIR='$SPEX' @rd_line.par linstr_spex=rd_line_linstr
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Ссылки http://hea-www.harvard.edu/PINTofALE/doc/TIP_DB_CHANGE -- 1.2 Кб -- 30.01.2001
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7327. http://hea-www.harvard.edu/PINTofALE/pro/id2emis2id.pro
function id2emis2id, idstr , ldbdir , dWVL = dWVL , verbose = verbose , _extra=e ;+ ;function id2emis2id ; takes an ID structure, strips it into component parts, ; reads in new emissivities, and puts them back in. ; ;syntax ; newidstr=id2emis2id( idstr , ldbdir , dWVL = dWVL , verbose = verbose ,$ ; eps=eps,/incieq,mapping=mapping,pres=pres,logP=logP,n_e=n_e,$ ; chifil=chifil,chidir=chidir,eqfile=eqfile) ; ;warning ; new ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/id2emis2id.pro -- 7.4 Кб -- 29.01.2001
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7328. http://hea-www.harvard.edu/PINTofALE/pro/drat.pro
function drat, line1 , line2 , edens , DEM , logT , fx1 = fx1 , fx2 = fx2 , _ extra =e ;+ ;function drat ; return the ratio of fluxes in one line relative to another line ; for a variety of densities ; ;syntax ; frat=drat( line1 , line2 , edens , DEM , logT , fx1 = fx1 , fx2 = ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/drat.pro -- 4.6 Кб -- 28.01.2001
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7329. http://hea-www.harvard.edu/PINTofALE/pro/cut_id.pro
... IDX+1) ; * if float, assumed to refer to IDSTR.( ... IDX +1) idxtr= idstr .( idx [0]+1L) ncomp= n_elements (idxtr.WVL) tnam =tag_names(idxtr) nflds= n_elements ( tnam ) for i=0,nflds-1 do begin if tnam [i] eq 'WVL' then xWVL=idxtr.WVL if tnam [i] eq 'Z' then xZ=idxtr.Z if tnam [i] eq 'ION' then xION=idxtr.ION if tnam [i] eq 'LABL' then xLABL =idxtr.LABL if tnam [i] eq 'FLUX' then xFLUX=idxtr.FLUX if tnam [i] eq 'FLUXERR' then xFLUXERR=idxtr.FLUXERR if ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/cut_id.pro -- 9.3 Кб -- 28.01.2001
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7330. http://hea-www.harvard.edu/PINTofALE/pro/linespec_em.pro
function linespec_em,atom, wmin = wmin , wmax = wmax , nbin = nbin ,wlog=wlog,ww=ww,$ ikev=ikev, fstr = fstr , tlog = tlog ,EM=EM, _extra=e ;+ ;function linespec_em ; returns a spectrum of atomic lines for a 1-T EM. output will be in ; units of [erg,ph]/s/cm^2/[keV,Ang] ; ; if IKEV is set , WMIN , WMAX ,WW must be input in [keV] and the ; output will have units .../keV ; ; if NOPH is ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/linespec_em.pro -- 6.6 Кб -- 25.01.2001
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7331. http://hea-www.harvard.edu/PINTofALE/pro/linespec.pro
function linespec,atom, wmin = wmin , wmax = wmax , nbin = nbin ,wlog=wlog,ww=ww,$ ikev = ikev , fstr = fstr , _extra=e ;+ ;function linespec ; returns a spectrum of atomic lines. output will be in units ; of [erg,ph]/s/cm^2/[keV,Ang] ; ; if IKEV is set , WMIN , WMAX ,WW must be input in [keV] and the ; output will have units .../keV ; ; if NOPH is set , output will have units of erg/... ; ; if EFFAR and WVLAR are not ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/linespec.pro -- 6.8 Кб -- 25.01.2001
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7332. http://hea-www.harvard.edu/PINTofALE/pro/flux_to_em.pro
function flux _to_em, emis , flux = flux , logT = logT , wvl = wvl ,Z=Z,NH=NH,defEM=defEM,$ noph=noph, thresh = thresh , _extra=e ;+ ;function flux _to_em ; return emission measures (-1 where undeterminable) at various ; temperatures consistent with given line fluxes and line emissivities. ; ; for each temperature, assume a delta-function emission measure, ; compute ...
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Ссылки http://hea-www.harvard.edu/PINTofALE/pro/flux_to_em.pro -- 6.0 Кб -- 24.01.2001
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7333. http://hea-www.harvard.edu/~bradw/cv/papers/CXwinds.ps
... Existing measurements of winds only apply to highґmass O and B stars, red giants, and supergiants and only extend down to a few times 10 #10 yr #1 , as compared to the M, solar rate of # yr #1 . ... Recent Xґray detections of comets suggest that charge transfer between highly charged ions in the solar wind and neutral gases in cometary atmospheres is responsible for much or all of the observed emission, a hypothesis that has been strengthened by Chandra observations of comet C/1999 S4 (LINEAR). ...
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Ссылки http://hea-www.harvard.edu/~bradw/cv/papers/CXwinds.ps -- 184.8 Кб -- 23.01.2001
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7334. http://hea-www.harvard.edu/~bradw/cv/papers/CXwinds.pdf
... We propose a novel method of studying stellar winds through obser vation of charge exchangeґinduced X-ray emission. Recent X-ray detections of comets suggest that charge transfer between highly charged ions in the solar wind and neutral gases in cometar y atmospheres is responsible for much or all of the obser ved emission, a hypothesis that has been strengthened by Chandra obser vations of comet C/1999 S4 (LINEAR). ... Likewise, the example wind can be seen at distances well beyond 10 pc. ...
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Ссылки http://hea-www.harvard.edu/~bradw/cv/papers/CXwinds.pdf -- 67.0 Кб -- 23.01.2001
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7335. http://hea-www.harvard.edu/~bradw/cv/papers/NeKLL.ps.gz
... The KLL dielectronic recombination satellites were resolved from their Heґlike parent lines in electron energy space, and their wavelengths and resonance strengths measured. ... By normalizing to the Heґlike resonance line, w, we measure Liґlike satellite resonance strengths that are 10% to 46% lower than predicted by theoretical models. ... 15# For unresolved satellites, G s is an average for the blended lines, weighted by their theoretical resonance strengths. ...
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Ссылки http://hea-www.harvard.edu/~bradw/cv/papers/NeKLL.ps.gz -- 127.7 Кб -- 17.01.2001
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7336. http://hea-www.harvard.edu/~bradw/cv/papers/NeKLL.pdf
... The KLL dielectronic recombination satellites were resolved from their He-like parent lines in electron energy space, and their wavelengths and resonance strengths measured. ... By normalizing to the He-like resonance line, w, we measure Li-like satellite resonance strengths that are 10% to 46% lower than predicted by theoretical models. ... 15 For unresolved satellites, G s is an average for the blended lines, weighted by their theoretical resonance strengths. ...
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Ссылки http://hea-www.harvard.edu/~bradw/cv/papers/NeKLL.pdf -- 147.2 Кб -- 17.01.2001
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7337. http://hea-www.harvard.edu/~pgreen/vitanew_old/vitanew.ps
... 1999, ApJ , 117, 707, BVRI Light Curves for 22 Type Ia Supernovae ffl Ralf Napiwotzki, Paul J. Green , Rex A. Saffer 1999, ApJ , 517, 399 A Comparative Study of the Mass Distribution of Extreme UltravioletґSelected White Dwarfs ffl Belinda J. Wilkes, J. Kuraszkiewicz, Paul J. Green , S. Mathur, J.C. McDowell 1999, ... Amer. Astron. ... P. J. Green 1997, Bull. ... Society, 25, 868. ffl ``On the Binarity of Dwarf Carbon Stars,'' P. J. Green and B. Margon 1993, Bull. ...
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Ссылки http://hea-www.harvard.edu/~pgreen/vitanew_old/vitanew.ps -- 199.7 Кб -- 15.01.2001
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7338. http://hea-www.harvard.edu/~pgreen/HRCULES/table2.ps
TABLE 2 Partial correlations All data (including upper limits) Detections only Line logW ? vs. log L 2500 logW ? vs. log z logW ? vs. log L 2500 logW ? vs. log z P ae P ae P ae P ae LBQS Sample Fe UV 0.177 ґ0.033 !0.005 ґ0.123 0.175 ґ0.983 0.175 ґ0.983 Lyfi+OVI .. ... C III] 0.066 0.060 0.011 ґ0.091 .. ... 18:6 Subsample Fe UV 0.177 ґ0.033 !0.005 ґ0.123 0.244 ґ0.030 0.208 ґ0.037 Lyff !0.005 0.379 !0.005 ґ0.446 !0.005 0.161 !0.005 ґ0.258 Si IV + OIV] .. ...
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Ссылки http://hea-www.harvard.edu/~pgreen/HRCULES/table2.ps -- 68.2 Кб -- 27.12.2000
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7339. http://hea-www.harvard.edu/~pgreen/HRCULES/table3.ps
TABLE 3 Evolution Regressions for LBQS Emission Lines Emission line All Data (including upper limits) Detections only NAME TOT UPP C/K/S a Slope Intercept NUM C/K/S Slope Intercept Full LBQS Fe UV 953 294 0.00 / 0.00 / 0.00 ґ1.312\Sigma0.101 1.13\ Sigma0.03 659 0.00 / 0.00 / 0.00 ґ0.190\Sigma0.038 1.52\ Sigma0.01 Lyff 259 0 0.00 / 0.00 / 0.00 ґ1.199\Sigma0.227 2.19\Sigma0.08 259 0.00 / 0.00 / ... 1% in all 3 correlation tests using all data, and an upper limit fraction ! ...
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Ссылки http://hea-www.harvard.edu/~pgreen/HRCULES/table3.ps -- 71.5 Кб -- 27.12.2000
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7340. http://hea-www.harvard.edu/~pgreen/HRCULES/table1.ps
TABLE 1 Baldwin Effect Regressions for the LBQS Emission line All Data (including upper limits) Detections only Line Name N T ot N Limits C/K/S a Slope Intercept N C/K/S a Slope Intercept Fe II UV 953 294 0.00 / 0.00 / 0.00 ґ0.617 \Sigma0.047 20.2 \ Sigma 1.4 659 0.00 / 0.00 / 0.00 ґ0.105 \ Sigma 0.016 4.8 \ Sigma 0.5 Fe II opt 248 110 0.00 / 0.00 / 0.00 ґ0.447 \ Sigma 0.108 14.5 \ ... The Baldwin effect examined here is log L 2500 / log W ? (line). ...
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Ссылки http://hea-www.harvard.edu/~pgreen/HRCULES/table1.ps -- 96.3 Кб -- 27.12.2000
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