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‹intestazione›
‹data/ora›<= span style=3D'font-size:67%;mso-special-format:lastCR'>
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------=_NextPart_01C8989C.EBC0A450 Content-Location: file:///C:/224830C1/marcacci_termodinamica_file/pres.xml Content-Transfer-Encoding: quoted-printable Content-Type: text/xml; charset="utf-8" ------=_NextPart_01C8989C.EBC0A450 Content-Location: file:///C:/224830C1/marcacci_termodinamica_file/slide0001.htm Content-Transfer-Encoding: quoted-printable Content-Type: text/html; charset="us-ascii" Calore ed energia: breve storia della termodinamica.
Calore ed energia: breve storia della termodinamica.
Storia del Pensiero Scientifico II, a.a. 2007/2008
Docente Flavia Marca= cci
Bibliografia
Y. Elkana, La scoperta della conservazione dell’energia, Feltrinelli, Milano 1977.
V. Bacciarelli – P. A. Giustini, Immagini del mondo fisico, vol. 2°, Trevisini = Editore, Milano 1988. <= /span>
E. Bellone, Cao= s e armonia, UTET, To= rino 2004.
M. Guillen, Le cinque equazioni che hanno cambiato il mondo. Potere e poesia = della matematica, TEA, Milano 1997
NB. Il materiale qui illustrato è ad uso strettamente didattico e non utilizzabile ad al= tri scopi.
Ultima revisione 4/4/2008
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Indice
•Parte I: I precedenti storici della termodinamica (diapositive 3-26)<= /span>= 3;•Parte II: I principi della termodinamica (diapositive 27-44) •Parte III: <= span style=3D'font-size:113%;color:white;mso-color-index:0'>Teoria cinetica, probabilità, termodinamica (diapositive 45-54)=
•Termini e concet= ti (diapositiva 53)
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I precedenti storici della <= /span>termodinamica
Parte I
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Prime concezioni
= sulla natura del calore: teoria dinamica contro teoria materiale
•<= /span>Antichità: calore come “stato” = o come “sostanza”
•<= /span>Galilei: «Poichè dunque ad eccitare il caldo non basta la presenza degl’ignicoli, ma ci vuole il loro movimento= ancora, qu= indi pare a me che non fosse se non con gran ragione detto il moto e= sser causa di calore» (Il Saggiatore)
•<= /span>àteoria dinamica del calore (basata sul movimento degl= i “ign= icoli”): sostenuta, oltre che da Galilei, da Hooke, Boyle, Loc= ke, Bacone, Keplero, Cartesio, Mariotte, Euler.
•<= /span>Seconda metà del XVIII: l’opposizione dei chimici à Black e la teoria “sostanziale” (o materi= ale) del calore.
•<= /span>Lavoisier definisce “calorico” questa sostanza.
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•Tentativi di conciliazione
•
•Laplace e Lavois= er, Mémoire sur la chaleur, 1780:
– I fisici sono divisi sulla natura del calore. Molti fra loro lo considerano un fluido diffuso nell’intera natura e da cui i= corpi sono più o meno penetrati, in ragione della loro temperatura e della loro disposizione = particolare a conservarlo… altri fisici pens= ano che il calore non sia altro che il risultato dei movimenti insensibili delle molecole della materia…= secondo i fisici di cui stiamo parlando, è = questo il movimento interno a costituire il calore.
Dopodichè veniva richiamato un principio comune ad entrambe le teorie:
La quantità di cal= ore libero rimane sempre la medesima nella semplice mescolanza dei corpi.
Infatti continua a valere la legge di conservazio= ne della vis viva<= /span> (Leibniz), cioè che della quantità (½)mv2.
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Il calorico
•<= /span>Fluido elastico e senza peso
•<= /span>Le sue particelle erano autorepulsive: questa forza era in grado di controbilanciare l’attrazione gravita= zionale evitando il collasso dei corpi in una massa solida omogenea (+ stabilità delle = atmosfere).
•<= /span>Fluido capace di penetrare nella materia e = = diffuso in essa.
•<= /span>Problemi risolti: spiegazione della contrazione e = <= span style=3D'font-size:88%'>dilatazione dei corpi e dei cambiamenti di stato.<= /span>
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Le t= eorie spiegate con il calorico
•<= /span>Cambiamenti di stato:
–Ghiaccio + calorico =3D acqua
–Acqua + calorico =3D vapor d’acqua
–
•<= /span>La densità della nube di calorico che circo= nda ogni atomo diminuisce in ragione di 1/rn = (n>2). Ovvero più rapidamente dell’azione gravitazionale à l’azione del calorico è a breve raggio.
•<= /span>Individuazione dello zero in una scala di temperature
•<= /span>1730-50: esperimenti di Boerhaave e Fahrenheit su liquidi a diversa temperature tra loro mescolati:
»
J. Bl= ack e la chiarificazione di alcuni termini (basandosi sulla teoria materiale):&#= 13;
• capacità termica specifica
•Distinzione tra calore latente (=3D non osse= rvabile per mezzo di termometri) e calore libero = (prodotto da particelle libere di muoversi c= on elevatissime velocità nello spazio tra le molecole): la loro somma era il calore assol= uto (àmodello a due discreti di Laplace).
•“temperatura” =3D intensit&agrav= e; del calore (libero)
•calorico come quantità di calore<= /b>
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Il calo= rico in formule
= •Legge di conservazione <= span style=3D'font-size:71%'>(calorimetria elementare): = il calore guadagnato da = un corpo è uguale al = calore perduto dall’altro = corpo.
Contenuto di calore del corpo =
dove c(T) è la capacità termica, T0<= /span> una qualsiasi temperatura standard e L è il calore latente.
NB: quantità di calore =3D prodotto della m= assa per la temperatura 
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Leggi macroscopiche
dei gas perfetti
•<= /span>Legge di Boyle Mariotte: in prima approssimazione = il prodotto tra la pressio= ne e il volume di un campione di gas è costante quando è <= /span>= costante la temperatura. PV=3Dk.
•<= /span>Gas perfetto: segue la legge di Boyle-Mariotte = ;
•<= /span>Legge di Charles-Gay Lussac, dove γ= ;0 è pari= a 1/273 (coefficiente di dilatazione cubica dei gas a 0°C), a pressione costante:
•Legge di Volta-Gay Lussac, a volume costante:
Per Vt<= /span>à0 tà-273&d= eg;C.
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La trattazione di Laplace
•<= /span>Tra meccanicismo e probabilità. =
•<= /span>Probabilità: la probabilità di un ev= ento è il rapporto tra il numero di casi che gli sono favorevoli e il numero di tutti i casi possibili, quando nulla porta a credere che si debba verificare uno di essi piuttosto che altri, il che li rende per noi ugualmente possibili <= span style=3D'font-family:Wingdings;font-size:59%;mso-char-type:symbol'>à= ; uniformare fenomeni complessi a poche cause e leggi: l’approssim= azione non è incertezza.
•<= /span>La conoscenza completamente determinata (sul model= lo dell’astronomia): allontanarsi dal falso per progredire verso il vero (fig. sotto).
•<= /span>Modello di Laplace per i gas: ogni molecole &egrav= e; un centro di irraggiamento e assorbimento. Essa è circondata da una atmosfera di <= span style=3D'position:absolute;top:54.25%;left:8.98%;width:97.0%;height:4.25%'= >calorico. Muovendosi tra le altre molecole, perde o attira particelle, in modo t= ale che il numero di particelle legate alla molecola resti costante nel tempo. Le particelle legate alle molecole sono= il calorico latente, quelle libero il = calorico libero. In questo modello agiscono forze newtoniane tra molecole ma anche forze a breve rag= gio d’azione tra moleco= le e particelle (cf. Bellone (2004), pp. 141-142) à distacco dal modello newtoniano e spiegazione di comportamenti macroscopici dei <= span style=3D'position:absolute;top:77.75%;left:8.98%;width:84.45%;height:4.25%= '>gas.
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